Open Access
Open access
Progress of Theoretical and Experimental Physics

Probing Cosmic Inflation with the LiteBIRD Cosmic Microwave Background Polarization Survey

E. Allys 1
, 
K. Arnold 2
, 
J. Aumont 3
, 
R. Aurlien 4
, 
S. Azzoni 5, 6
, 
C. Baccigalupi 7, 8, 9
, 
A. J. Banday 3
, 
R BANERJI 4
, 
R. B. Barreiro 10
, 
N. BARTOLO 11, 12, 13
, 
L. Bautista 3
, 
D. Beck 14
, 
S. Beckman 15
, 
M. Bersanelli 16, 17
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F. Boulanger 1
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M. Brilenkov 4
, 
M. Bucher 18
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E. Calabrese 19
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P Campeti 20
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A Carones 21, 22
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F J Casas 10
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A. Catalano 23
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V. CHAN 24
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K. Cheung 15, 25, 26
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Y. Chinone 6, 27
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S E Clark 14, 28
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F Columbro 29, 30
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G D'Alessandro 29, 30
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P. De BERNARDIS 29, 30
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T. de Haan 31
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E De La Hoz 10, 32
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M. De Petris 29, 30
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S. Della Torre 33
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P Diego Palazuelos 10, 32
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M. Dobbs 34
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T. Dotani 35, 36
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J M Duval 37
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T. Elleflot 38
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H. K. Eriksen 4
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J. Errard 18
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T Essinger Hileman 39
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F. Finelli 40, 41
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R Flauger 2
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C. Franceschet 16, 17
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U. Fuskeland 4
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M. Galloway 4
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K. Ganga 18
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M. Gerbino 42
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M. Gervasi 33, 43
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R T Génova-Santos 44, 45
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T Ghigna 5, 6
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S Giardiello 46
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E. Gjerløw 4
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J. Grain 47
, 
F. Grupp 48
, 
A. Gruppuso 40, 41
, 
J. E. Gudmundsson 49
, 
N. W. Halverson 50
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P Hargrave 19
, 
T. Hasebe 6
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M Hasegawa 31, 36, 51
, 
M Hazumi 6, 31, 35, 36, 51
, 
S. Henrot-Versillé 52
, 
B. Hensley 53
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L T Hergt 54
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D. HERMAN 4
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E. Hivon 55
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R A Hlozek 24
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A L Hornsby 15
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Y. Hoshino 56
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J. Hubmayr 57
, 
K. Ichiki 58
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T Iida 59
, 
H Imada 60
, 
H. Ishino 61
, 
G. Jaehnig 50
, 
N Katayama 6
, 
A. Kato 31
, 
R. Keskitalo 15, 25, 26
, 
T. Kisner 26
, 
Y. Kobayashi 62
, 
A. Kogut 39
, 
K. Kohri 31
, 
E. Komatsu 6, 20
, 
K Komatsu 61
, 
K. Konishi 63
, 
N. Krachmalnicoff 7, 8, 9
, 
C. L. Kuo 14, 64
, 
L Lamagna 29, 30
, 
M. LATTANZI 42
, 
A. T. Lee 15, 38, 51
, 
C. Leloup 18
, 
F. Levrier 1
, 
E. Linder 25, 38
, 
G Luzzi 65
, 
J Macias Perez 23
, 
T. Maciaszek 66
, 
B Maffei 47
, 
D. Maino 16
, 
S Mandelli 16, 17
, 
E. Martínez-González 10
, 
S. Masi 29, 30
, 
M. Massa 67
, 
S. Matarrese 11, 12, 13, 68
, 
F T Matsuda 35
, 
T Matsumura 6
, 
L Mele 29, 30
, 
M. Migliaccio 21, 22
, 
Y. Minami 69
, 
A. Moggi 67
, 
J. Montgomery 34
, 
L. Montier 3
, 
G Morgante 40
, 
B. Mot 3
, 
Y Nagano 61
, 
T. Nagasaki 31
, 
R. Nagata 35
, 
R. Nakano 35, 70
, 
T. Namikawa 6
, 
F. Nati 33, 43
, 
P. Natoli 42, 46
, 
S Nerval 24
, 
F. Noviello 19
, 
K Odagiri 35
, 
S. Oguri 35
, 
H Ohsaki 62
, 
L. Pagano 42, 46, 47
, 
A Paiella 29, 30
, 
D. Paoletti 40, 41
, 
A. Passerini 33, 43
, 
G. Patanchon 18
, 
F. PIACENTINI 29, 30
, 
M. Piat 18
, 
G Pisano 19, 29, 30
, 
G. Polenta 65
, 
D. Poletti 33, 43
, 
T Prouvé 37
, 
G. Puglisi 21, 26
, 
D. Rambaud 3
, 
C Raum 15
, 
S. Realini 16
, 
M. Reinecke 20
, 
M. Remazeilles 10, 71
, 
A. Ritacco 1, 47, 72
, 
G. Roudil 3
, 
J.-A. Rubino-Martin 44, 45
, 
M Russell 2
, 
H. Sakurai 62
, 
Y Sakurai 6, 61
, 
M. Sasaki 73
, 
D. Scott 54
, 
Y. Sekimoto 31, 35, 70
, 
K. Shinozaki 74
, 
M. SHIRAISHI 75
, 
P Shirron 39
, 
G. Signorelli 67
, 
F. Spinella 67
, 
S Stever 6, 61
, 
R. Stompor 18, 76
, 
S. Sugiyama 56
, 
R M Sullivan 54
, 
A. Suzuki 26
, 
T. L. Svalheim 4
, 
E Switzer 39
, 
R Takaku 35, 77
, 
H. Takakura 35, 70
, 
Y. Takase 61
, 
A. Tartari 67, 78
, 
Y Terao 62
, 
J Thermeau 18
, 
H. Thommesen 4
, 
K. L. Thompson 14, 64
, 
M. Tomasi 16, 17
, 
M Tominaga 35, 70
, 
M. Tristram 52
, 
M. Tsuji 79
, 
M. Tsujimoto 35
, 
L Vacher 3
, 
P Vielva 10
, 
N. Vittorio 21, 22
, 
W. Wang 18
, 
K. Watanuki 35
, 
I. K. Wehus 4
, 
J. Weller 48
, 
B. Westbrook 15
, 
J. Wilms 73
, 
B. Winter 80, 81
, 
E J Wollack 39
, 
J Yumoto 62
, 
M. Zannoni 33, 43
Show full list: 190 authors
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IRAP, Université de Toulouse , (Toulouse), 9, avenue du Colonel Roche BP 44346 31028 Toulouse Cedex 4 , France | 
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Université de Paris, CNRS, Astroparticule et Cosmologie , F-75013 Paris , France | 
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David A. Dunlap Department of Astronomy and Astrophysics , 50 St George Street, Toronto, ON M5S 3H4 , Canada | 
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NIST Quantum Sensors Group, 325 Broadway, Boulder , CO 80305 , USA | 
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ispace, inc. , Tokyo 103-0007 , Japan | 
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Centre National d’Etudes Spatiales (CNES) , 18 avenue Edouard Belin 31 401 TOULOUSE CEDEX 4 , France | 
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School of General and Management Studies, Suwa University of Science , 5000-1 Toyohira, Chino, Nagano 391-0292 , Japan | 
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CNRS-UCB International Research Laboratory, Centre Pierre Binétruy , UMI2007, Berkeley, CA 94720 , USA | 
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National Institute of Technology, Kagawa College , Kagawa 761-8058 , Japan | 
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Publication type: Journal Article
Publication date: 2022-11-21
scimago Q1
SJR: 2.483
CiteScore: 12.0
Impact factor: —
ISSN: 20503911
Abstract

LiteBIRD the Lite (Light) satellite for the study of B-mode polarization and Inflation from cosmic background Radiation Detection, is a space mission for primordial cosmology and fundamental physics. The Japan Aerospace Exploration Agency (JAXA) selected LiteBIRD in May 2019 as a strategic large-class (L-class) mission, with an expected launch in the late 2020s using JAXA’s H3 rocket. LiteBIRD is planned to orbit the Sun-Earth Lagrangian point L2, where it will map the cosmic microwave background (CMB) polarization over the entire sky for three years, with three telescopes in 15 frequency bands between 34 and 448 GHz, to achieve an unprecedented total sensitivity of 2.2 μK-arcmin, with a typical angular resolution of 0.5○ at 100 GHz. The primary scientific objective of LiteBIRD is to search for the signal from cosmic inflation, either making a discovery or ruling out well-motivated inflationary models. The measurements of LiteBIRD will also provide us with insight into the quantum nature of gravity and other new physics beyond the standard models of particle physics and cosmology. We provide an overview of the LiteBIRD project, including scientific objectives, mission and system requirements, operation concept, spacecraft and payload module design, expected scientific outcomes, potential design extensions and synergies with other projects. Subject Index LiteBIRD cosmic inflation, cosmic microwave background, B-mode polarization, primordial gravitational waves, quantum gravity, space telescope

Found 495
By date By citations
IOP Publishing
New constraints on axion-gauge field dynamics during inflation from Planck and BICEP/Keck data sets
Campeti P., Özsoy O., Obata I., Shiraishi M.
Journal of Cosmology and Astroparticle Physics scimago Q2 wos Q1 , 
2022-07-01,  citations by CoLab: 17 ,  Abstract  
Abstract We present new constraints on spectator axion-U(1) gauge field interactions during inflation using the latest Planck (PR4) and BICEP/Keck 2018 data releases. This model can source tensor perturbations from amplified gauge field fluctuations, driven by an axion rolling for a few e-folds during inflation. The gravitational waves sourced in this way have a strongly scale-dependent (and chiral) spectrum, with potentially visible contributions to large/intermediate scale B-modes of the CMB. We first derive theoretical bounds on the model imposing validity of the perturbative regime and negligible backreaction of the gauge field on the background dynamics. Then, we determine bounds from current CMB observations, adopting a frequentist profile likelihood approach. We study the behaviour of constraints for typical choices of the model's parameters, analyzing the impact of different dataset combinations. We find that observational bounds are competitive with theoretical ones and together they exclude a significant portion of the model's parameter space. We argue that the parameter space still remains large and interesting for future CMB experiments targeting large/intermediate scales B-modes.
Springer Nature
New physics from the polarized light of the cosmic microwave background
Komatsu E.
Nature Reviews Physics scimago Q1 wos Q1 , 
2022-05-18,  citations by CoLab: 95 ,  Abstract  
The current cosmological model requires new physics beyond the standard model of elementary particles and fields, such as dark matter and dark energy. Their nature is unknown and so is that of the initial fluctuations in the early Universe that led to the creation of the cosmic structure we see today. Polarized light of the cosmic microwave background (CMB) may hold the answer to these fundamental questions. Here, I discuss two phenomena that could be uncovered in CMB observations. First, if the physics behind dark matter and dark energy violates parity symmetry, their coupling to photons should have rotated the plane of linear polarization as the CMB photons have been travelling for more than 13 billion years. This effect is known as ‘cosmic birefringence’. A tantalizing hint of such a signal has been found with a statistical significance of 3σ. Second, the period of accelerated expansion in the very early Universe, called ‘cosmic inflation’, might have produced a stochastic background of primordial gravitational waves (as yet unobserved). These might have been generated by vacuum fluctuations in spacetime or by matter fields and could be measurable in the CMB polarization. The goal of observing these two phenomena will influence how data from future CMB experiments are collected, calibrated and analysed. The polarization of the cosmic microwave background (CMB) may shed light on the nature of dark matter and dark energy, and on the origin of all structures in the Universe. Discovering a signature of such new physics in the CMB will require new observational and calibration strategies for future CMB experiments.
American Physical Society (APS)
Improved limits on the tensor-to-scalar ratio using BICEP and Planck data
Tristram M., Banday A. ., Górski K. ., Keskitalo R., Lawrence C. ., Andersen K. ., Barreiro R. ., Borrill J., Colombo L. ., Eriksen H. ., Fernandez-Cobos R., Kisner T. ., Martínez-González E., Partridge B., Scott D., et. al.
Physical Review D scimago Q1 wos Q1 , 
2022-04-26,  citations by CoLab: 148 ,  Abstract  
We present constraints on the tensor-to-scalar ratio $r$ using a combination of BICEP/Keck 2018 (BK18) and Planck PR4 data allowing us to fit for $r$ consistently with the six parameters of the $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$ model. We discuss the sensitivity of constraints on $r$ to uncertainties in the $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$ parameters as defined by the Planck data. In particular, we are able to derive a constraint on the reionization optical depth $\ensuremath{\tau}$ and thus propagate its uncertainty into the posterior distribution for $r$. While Planck sensitivity to $r$ is slightly lower than the current ground-based measurements, the combination of Planck with BK18 and baryon-acoustic-oscillation data yields results consistent with $r=0$ and tightens the constraint to $r<0.032$ at 95% confidence.
American Astronomical Society
The Simons Observatory: Galactic Science Goals and Forecasts
Hensley B.S., Clark S.E., Fanfani V., Krachmalnicoff N., Fabbian G., Poletti D., Puglisi G., Coppi G., Nibauer J., Gerasimov R., Galitzki N., Choi S.K., Ashton P.C., Baccigalupi C., Baxter E., et. al.
Astrophysical Journal scimago Q1 wos Q1 Open Access , 
2022-04-01,  citations by CoLab: 19 ,  Abstract  
Abstract Observing in six frequency bands from 27 to 280 GHz over a large sky area, the Simons Observatory (SO) is poised to address many questions in Galactic astrophysics in addition to its principal cosmological goals. In this work, we provide quantitative forecasts on astrophysical parameters of interest for a range of Galactic science cases. We find that SO can: constrain the frequency spectrum of polarized dust emission at a level of Δβ d ≲ 0.01 and thus test models of dust composition that predict that β d in polarization differs from that measured in total intensity; measure the correlation coefficient between polarized dust and synchrotron emission with a factor of two greater precision than current constraints; exclude the nonexistence of exo-Oort clouds at roughly 2.9σ if the true fraction is similar to the detection rate of giant planets; map more than 850 molecular clouds with at least 50 independent polarization measurements at 1 pc resolution; detect or place upper limits on the polarization fractions of CO(2–1) emission and anomalous microwave emission at the 0.1% level in select regions; and measure the correlation coefficient between optical starlight polarization and microwave polarized dust emission in 1° patches for all lines of sight with N H ≳ 2 × 1020 cm−2. The goals and forecasts outlined here provide a roadmap for other microwave polarization experiments to expand their scientific scope via Milky Way astrophysics. 37 37 A supplement describing author contributions to this paper can be found at https://simonsobservatory.org/wp-content/uploads/2022/02/SO_GS_Contributions.pdf.
American Astronomical Society
A Constraint on Primordial B-modes from the First Flight of the Spider Balloon-borne Telescope
Ade P.A., Amiri M., Benton S.J., Bergman A.S., Bihary R., Bock J.J., Bond J.R., Bonetti J.A., Bryan S.A., Chiang H.C., Contaldi C.R., Doré O., Duivenvoorden A.J., Eriksen H.K., Farhang M., et. al.
Astrophysical Journal scimago Q1 wos Q1 Open Access , 
2022-03-01,  citations by CoLab: 39 ,  Abstract  
Abstract We present the first linear polarization measurements from the 2015 long-duration balloon flight of Spider, which is an experiment that is designed to map the polarization of the cosmic microwave background (CMB) on degree angular scales. The results from these measurements include maps and angular power spectra from observations of 4.8% of the sky at 95 and 150 GHz, along with the results of internal consistency tests on these data. While the polarized CMB anisotropy from primordial density perturbations is the dominant signal in this region of sky, Galactic dust emission is also detected with high significance. Galactic synchrotron emission is found to be negligible in the Spider bands. We employ two independent foreground-removal techniques to explore the sensitivity of the cosmological result to the assumptions made by each. The primary method uses a dust template derived from Planck data to subtract the Galactic dust signal. A second approach, which constitutes a joint analysis of Spider and Planck data in the harmonic domain, assumes a modified-blackbody model for the spectral energy distribution of the dust with no constraint on its spatial morphology. Using a likelihood that jointly samples the template amplitude and r parameter space, we derive 95% upper limits on the primordial tensor-to-scalar ratio from Feldman–Cousins and Bayesian constructions, finding r < 0.11 and r < 0.19, respectively. Roughly half the uncertainty in r derives from noise associated with the template subtraction. New data at 280 GHz from Spider’s second flight will complement the Planck polarization maps, providing powerful measurements of the polarized Galactic dust emission.
American Physical Society (APS)
Cosmic Birefringence from the Planck Data Release 4
Diego-Palazuelos P., Eskilt J. ., Minami Y., Tristram M., Sullivan R. ., Banday A. ., Barreiro R. ., Eriksen H. ., Górski K. ., Keskitalo R., Komatsu E., Martínez-González E., Scott D., Vielva P., Wehus I. .
Physical Review Letters scimago Q1 wos Q1 Open Access , 
2022-03-01,  citations by CoLab: 96 ,  Abstract  
We search for the signature of parity-violating physics in the cosmic microwave background, called cosmic birefringence, using the Planck data release 4. We initially find a birefringence angle of $\ensuremath{\beta}=0.30\ifmmode^\circ\else\textdegree\fi{}\ifmmode\pm\else\textpm\fi{}0.11\ifmmode^\circ\else\textdegree\fi{}$ (68% C.L.) for nearly full-sky data. The values of $\ensuremath{\beta}$ decrease as we enlarge the Galactic mask, which can be interpreted as the effect of polarized foreground emission. Two independent ways to model this effect are used to mitigate the systematic impact on $\ensuremath{\beta}$ for different sky fractions. We choose not to assign cosmological significance to the measured value of $\ensuremath{\beta}$ until we improve our knowledge of the foreground polarization.
American Astronomical Society
CMB/kSZ and Compton-y Maps from 2500 deg2 of SPT-SZ and Planck Survey Data
Bleem L.E., Crawford T.M., Ansarinejad B., Benson B.A., Bocquet S., Carlstrom J.E., Chang C.L., Chown R., Crites A.T., Haan T.D., Dobbs M.A., Everett W.B., George E.M., Gualtieri R., Halverson N.W., et. al.
Astrophysical Journal, Supplement Series scimago Q1 wos Q1 Open Access , 
2022-02-01,  citations by CoLab: 37 ,  Abstract  
Abstract We present component-separated maps of the primary cosmic microwave background/kinematic Sunyaev–Zel’dovich (SZ) amplitude and the thermal SZ Compton-y parameter, created using data from the South Pole Telescope (SPT) and the Planck satellite. These maps, which cover the ∼2500 deg2 of the southern sky imaged by the SPT-SZ survey, represent a significant improvement over previous such products available in this region by virtue of their higher angular resolution ( 1 .′ 25 for our highest-resolution Compton-y maps) and lower noise at small angular scales. In this work we detail the construction of these maps using linear combination techniques, including our method for limiting the correlation of our lowest-noise Compton-y map products with the cosmic infrared background. We perform a range of validation tests on these data products to test our sky modeling and combination algorithms, and we find good performance in all of these tests. Recognizing the potential utility of these data products for a wide range of astrophysical and cosmological analyses, including studies of the gas properties of galaxies, groups, and clusters, we make these products publicly available at http://pole.uchicago.edu/public/data/sptsz_ymap and on the NASA/LAMBDA website.
SPIE-Intl Soc Optical Eng
Performance and characterization of the SPT-3G digital frequency-domain multiplexed readout system using an improved noise and crosstalk model
Montgomery J., Ade P.A., Ahmed Z., Anderes E., Anderson A.J., Archipley M., Avva J.S., Aylor K., Balkenhol L., Barry P.S., Thakur R.B., Benabed K., Bender A.N., Benson B.A., Bianchini F., et. al.
Journal of Astronomical Telescopes, Instruments, and Systems scimago Q2 wos Q3 , 
2022-01-08,  citations by CoLab: 9 ,  Abstract  
The third generation South Pole Telescope camera (SPT-3G) improves upon its predecessor (SPTpol) by an order of magnitude increase in detectors on the focal plane. The technology used to read out and control these detectors, digital frequency-domain multiplexing (DfMUX), is conceptually the same as used for SPTpol, but extended to accommodate more detectors. A nearly 5x expansion in the readout operating bandwidth has enabled the use of this large focal plane, and SPT-3G performance meets the forecasting targets relevant to its science objectives. However, the electrical dynamics of the higher-bandwidth readout differ from predictions based on models of the SPTpol system due to the higher frequencies used, and parasitic impedances associated with new cryogenic electronic architecture. To address this, we present an updated derivation for electrical crosstalk in higher-bandwidth DfMUX systems, and identify two previously uncharacterized contributions to readout noise, which become dominant at high bias frequency. The updated crosstalk and noise models successfully describe the measured crosstalk and readout noise performance of SPT-3G. These results also suggest specific changes to warm electronics component values, wire-harness properties, and SQUID parameters, to improve the readout system for future experiments using DfMUX, such as the LiteBIRD space telescope.
EDP Sciences
Detailed study of HWP non-idealities and their impact on future measurements of CMB polarization anisotropies from space
Giardiello S., Gerbino M., Pagano L., Errard J., Gruppuso A., Ishino H., Lattanzi M., Natoli P., Patanchon G., Piacentini F., Pisano G.
Astronomy and Astrophysics scimago Q1 wos Q1 , 
2021-11-05,  citations by CoLab: 12 ,  Abstract  
We study the propagation of a specific class of instrumental systematics to the reconstruction of the B-mode power spectrum of the cosmic microwave background (CMB). We focus on the non-idealities of the half-wave plate (HWP), a polarization modulator that is to be deployed by future CMB experiments, such as the phase-A satellite mission LiteBIRD. We study the effects of non-ideal HWP properties, such as transmittance, phase shift, and cross-polarization. To this end, we developed a simple, yet stand-alone end-to-end simulation pipeline adapted to LiteBIRD. We analyzed the effects of a possible mismatch between the measured frequency profiles of HWP properties (used in the mapmaking stage of the pipeline) and the actual profiles (used in the sky-scanning step). We simulated single-frequency, CMB-only observations to emphasize the effects of non-idealities on the BB power spectrum. We also considered multi-frequency observations to account for the frequency dependence of HWP properties and the contribution of foreground emission. We quantified the systematic effects in terms of a bias Δr on the tensor-to-scalar ratio, r, with respect to the ideal case without systematic effects. We derived the accuracy requirements on the measurements of HWP properties by requiring Δr < 10−5 (1% of the expected LiteBIRD sensitivity on r). Our analysis is introduced by a detailed presentation of the mathematical formalism employed in this work, including the use of the Jones and Mueller matrix representations.
EDP Sciences
Development and application of metamaterial-based half-wave plates for the NIKA and NIKA2 polarimeters
Pisano G., Ritacco A., Monfardini A., Tucker C., Ade P.A., Shitvov A., Benoit A., Calvo M., Catalano A., Goupy J., Leclercq S., Macias-Perez J., Andrianasolo A., Ponthieu N.
Astronomy and Astrophysics scimago Q1 wos Q1 , 
2021-11-03,  citations by CoLab: 10 ,  Abstract  
Context. Large field-of-view imaging and polarimetry instruments operating at millimetre and sub-millimetre wavelengths are fundamental tools to understand the role of magnetic fields in channelling filament material into prestellar cores, providing unique insight in the physics of galactic star-forming regions. Among other topics, at extra-galactic scales, polarisation observations of Active Galactic Nuclei (AGNs) will allow us to constrain the possible physical conditions of the emitting plasma from the jets and/or explore the physics of dust inside supernova remnants. The kilo-pixel New IRAM KIDs Array 2 (NIKA2) camera, installed today at the Institut de Radioastronomie Millimétrique (IRAM) 30-m telescope, represents one of the best tools available to astronomers to produce simultaneous intensity and polarimetry maps over large fields at 260 GHz (1.15 mm). Aims. The polarisation measurement, in NIKA and NIKA2, is achieved by rapidly modulating the total incoming polarisation. In the end, this allows one to safely isolate the small science signal from the large, un-polarised, and strongly variable, atmospheric background. Methods. The polarisation modulation is achieved by inserting a fast rotating half-wave plate (HWP) in the optical beam. In order to allow wide field-of-view observations, the plate has to be large, with a diameter of 250 mm. The modulation of the polarised signal at 12 Hz also requires the waveplate to be sufficiently light. In addition, this key optical element has to exhibit optimal electromagnetic characteristics in terms of transmission and differential phase-shift. For this purpose, three metamaterial HWPs have been developed using the mesh-filter technology. The knowledge acquired in developing the first two single-band HWPs was used to achieve the more challenging performance requirements of the last dual-band HWP. The first and the third waveplates met the requirements for both the NIKA and NIKA2 instruments. Results. We first illustrate the design, the technical developments, the fabrication, and laboratory characterisation of the three mesh-HWPs. The deployment of two such elements in the NIKA and NIKA2 instruments at the 30-metre telescope is then described. We conclude with representative examples of astrophysical maps integrating polarimetry.
The Open Journal
The Python Sky Model 3 software
Zonca A., Thorne B., Krachmalnicoff N., Borrill J.
The Journal of Open Source Software Open Access , 
2021-11-01,  citations by CoLab: 22 , 
American Astronomical Society
The Crab Nebula as a Calibrator for Wide-beam Cosmic Microwave Background Polarization Surveys
Masi S., de Bernardis P., Columbro F., Coppolecchia A., D’Alessandro G., Mele L., Paiella A., Piacentini F.
Astrophysical Journal scimago Q1 wos Q1 Open Access , 
2021-10-28,  citations by CoLab: 5 ,  Abstract  
We analyze the effect of polarized diffuse emission in the calibration of wide-beam mm-wave polarimeters, when using the Crab Nebula as a reference source for both polarized brightness and polarization angle. We show that, for CMB polarization experiments aiming at detecting B-mode in a scenario with a tensor to scalar ratio $r \sim 0.001$, wide (a few degrees in diameter), precise ($\sigma_Q$ , $\sigma_U$ $\sim$ 20 $\mu$$K_{CMB}$ arcmin), high angular resolution ($< \mathrm{FWHM}$) reference maps are needed to properly take into account the effects of diffuse polarized emission and avoid significant bias in the calibration.
American Physical Society (APS)
Improved Constraints on Primordial Gravitational Waves using Planck , WMAP, and BICEP/ Keck Observations through the 2018 Observing Season
Ade P. ., Ahmed Z., Amiri M., Barkats D., Thakur R.B., Bischoff C. ., Beck D., Bock J. ., Boenish H., Bullock E., Buza V., Cheshire J. ., Connors J., Cornelison J., Crumrine M., et. al.
Physical Review Letters scimago Q1 wos Q1 Open Access , 
2021-10-04,  citations by CoLab: 609 ,  Abstract  
We present results from an analysis of all data taken by the BICEP2, Keck Array, and BICEP3 CMB polarization experiments up to and including the 2018 observing season. We add additional Keck Array observations at 220 GHz and BICEP3 observations at 95 GHz to the previous 95/150/220 GHz dataset. The Q/U maps now reach depths of 2.8, 2.8, and 8.8 μK_{CMB} arcmin at 95, 150, and 220 GHz, respectively, over an effective area of ≈600 square degrees at 95 GHz and ≈400 square degrees at 150 and 220 GHz. The 220 GHz maps now achieve a signal-to-noise ratio on polarized dust emission exceeding that of Planck at 353 GHz. We take auto- and cross-spectra between these maps and publicly available WMAP and Planck maps at frequencies from 23 to 353 GHz and evaluate the joint likelihood of the spectra versus a multicomponent model of lensed ΛCDM+r+dust+synchrotron+noise. The foreground model has seven parameters, and no longer requires a prior on the frequency spectral index of the dust emission taken from measurements on other regions of the sky. This model is an adequate description of the data at the current noise levels. The likelihood analysis yields the constraint r_{0.05}
Springer Nature
Ultra-light dark matter
Ferreira E.G.
Astronomy and Astrophysics Review scimago Q1 wos Q1 , 
2021-09-09,  citations by CoLab: 240 ,  Abstract  
Ultra-light dark matter is a class of dark matter models (DM), where DM is composed by bosons with masses ranging from $$10^{-24}\, \mathrm {eV}< m < \mathrm {eV}$$ . These models have been receiving a lot of attention in the past few years given their interesting property of forming a Bose–Einstein condensate (BEC) or a superfluid on galactic scales. BEC and superfluidity are some of the most striking quantum mechanical phenomena that manifest on macroscopic scales, and upon condensation, the particles behave as a single coherent state, described by the wavefunction of the condensate. The idea is that condensation takes place inside galaxies while outside, on large scales, it recovers the successes of $$\varLambda $$ CDM. This wave nature of DM on galactic scales that arise upon condensation can address some of the curiosities of the behaviour of DM on small-scales. There are many models in the literature that describe a DM component that condenses in galaxies. In this review, we are going to describe those models, and classify them into three classes, according to the different non-linear evolution and structures they form in galaxies: the fuzzy dark matter (FDM), the self-interacting fuzzy dark matter (SIFDM), and the DM superfluid. Each of these classes comprises many models, each presenting a similar phenomenology in galaxies. They also include some microscopic models like the axions and axion-like particles. To understand and describe this phenomenology in galaxies, we are going to review the phenomena of BEC and superfluidity that arise in condensed matter physics, and apply this knowledge to DM. We describe how ULDM can potentially reconcile the cold DM picture with the small-scale behaviour. These models present a rich phenomenology that is manifest in different astrophysical consequences. We review here the astrophysical and cosmological tests used to constrain those models, together with new and future observations that promise to test these models in different regimes. For the case of the FDM class, the mass where this model has an interesting phenomenology on small-scales $$ \sim 10^{-22}\, \mathrm {eV}$$ , is strongly challenged by current observations. The parameter space for the other two classes remains weakly constrained. We finalize by showing some predictions that are a consequence of the wave nature of this component, like the creation of vortices and interference patterns, that could represent a smoking gun in the search of these rich and interesting alternative class of DM models.
American Physical Society (APS)
Constraining reionization with the first measurement of the cross-correlation between the CMB optical-depth fluctuations and the Compton y -map
Namikawa T., Roy A., Sherwin B.D., Battaglia N., Spergel D.N.
Physical Review D scimago Q1 wos Q1 , 
2021-09-07,  citations by CoLab: 10 ,  Abstract  
We propose a new reionization probe that uses cosmic microwave background (CMB) observations; the cross-correlation between fluctuations in the CMB optical depth which probes the integrated electron density, $\delta\tau$, and the Compton $y$-map which probes the integrated electron pressure. This cross-correlation is much less contaminated than the $y$-map power spectrum by late-time cluster contributions. In addition, this cross-correlation can constrain the temperature of ionized bubbles while the optical-depth fluctuations and kinetic SZ effect can not. We measure this new observable using a Planck $y$-map as well as a map of optical-depth fluctuations that we reconstruct from Planck CMB temperature data. We use our measurements to derive a first CMB-only upper limit on the temperature inside ionized bubbles, $T_{\rm b}\lesssim 7.0\times10^5\,$K ($2\,\sigma$). We also present future forecasts, assuming a fiducial model with characteristic reionization bubble size $R_{\rm b}=5\,$Mpc and $T_{\rm b}=5\times10^4\,$K. The signal-to-noise ratio of the fiducial cross-correlation using a signal dominated PICO-like $y$-map becomes $\simeq7$ with CMB-S4 $\delta\tau$ and $\simeq13$ with CMB-HD $\delta\tau$. For the fiducial model, we predict that the CMB-HD $-$ PICO cross-correlation should achieve an accurate measurement of the reionization parameters; $T_{\rm b}\simeq 49800^{+4500}_{-5100}\,$K and $R_{\rm b}\simeq 5.09^{+0.66}_{-0.79}\,$Mpc. Since the power spectrum of the electron density fluctuations is constrained by the $\delta\tau$ auto spectrum, the temperature constraints should be only weakly model-dependent on the details of the electron distributions and should be statistically representative of the temperature in ionized bubbles during reionization. This cross-correlation could, therefore, become an important observable for future CMB experiments.
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American Physical Society (APS)
Signal-preserving CMB component separation with machine learning
McCarthy F., Hill J.C., Coulton W.R., Hogg D.W.
Physical Review D scimago Q1 wos Q1 , 
2025-03-28,  citations by CoLab: 0 ,  Abstract  
Analysis of microwave sky signals, such as the cosmic microwave background, often requires component separation using multifrequency methods, whereby different signals are isolated according to their different frequency behaviors. Many so-called blind methods, such as the internal linear combination (ILC), make minimal assumptions about the spatial distribution of the signal or contaminants, and only assume knowledge of the frequency dependence of the signal. The ILC produces a minimum-variance linear combination of the measured frequency maps. In the case of Gaussian, statistically isotropic fields, this is the optimal linear combination, as the variance is the only statistic of interest. However, in many cases the signal we wish to isolate, or the foregrounds we wish to remove, are non-Gaussian and/or statistically anisotropic (in particular for the case of Galactic foregrounds). In such cases, it is possible that machine learning (ML) techniques can be used to exploit the non-Gaussian features of the foregrounds and thereby improve component separation. However, many ML techniques require the use of complex, difficult-to-interpret operations on the data. We propose a hybrid method whereby we train an ML model using only combinations of the data that , and combine the resulting ML-predicted foreground estimate with the ILC solution to reduce the error from the ILC. We demonstrate our methods on simulations of extragalactic temperature and Galactic polarization foregrounds and show that our ML model can exploit non-Gaussian features, such as point sources and spatially varying spectral indices, to produce lower-variance maps than ILC—e.g., reducing the variance of the B-mode residual by factors of up to 5—while preserving the signal of interest in an unbiased manner. Moreover, we often find improved performance even when applying our ML technique to foreground models on which it was not trained. Published by the American Physical Society 2025
IOP Publishing
Rescaled Einstein-Gauss-Bonnet Gravity Inflation
Oikonomou V.K., Gkioni A., Sdranis I., Tsyba P., Razina O.
Classical and Quantum Gravity scimago Q1 wos Q2 , 
2025-03-28,  citations by CoLab: 0 ,  Abstract  
Abstract We study the inflationary phenomenology of a rescaled Einstein–Gauss–Bonnet (EGB) gravity. In this framework, the gravitational constant of the Einstein–Hilbert term is rescaled due to effective terms active in the high curvature era. Basically, the total theory is an F ( R , G , ϕ ) theory with the Gauss–Bonnet part contributing only a non-minimal coupling to the scalar field, so it is a theory with string theory origins and with a non-trivial F(R) gravity part. The F(R) gravity part in the high curvature regime contributes only a rescaled Einstein–Hilbert term and thus the resulting theory is effectively a rescaled version of a standard EGB theory. We develop the formalism of rescaled EGB gravity, taking in account the GW170817 constraints on the gravitational wave speed. We show explicitly how the rescaled theory affects directly the primordial scalar and tensor perturbations, and how the slow-roll and observational indices of inflation are affected by the rescaling of the theory. We perform a thorough phenomenological analysis of several models of interest and we show that is it possible to obtain viable inflationary theories compatible with the latest Planck data. Also among the studied models there are cases that yield a relatively large blue tilted tensor spectral index and we demonstrate that these models can lead to detectable primordial gravitational waves in the future gravitational wave experiments. Some of the scenarios examined, for specific values of the reheating temperature may be detectable by SKA, LISA, BBO, DECIGO and the Einstein Telescope.
American Physical Society (APS)
Square Kilometer Array as a cosmic microwave background experiment
Zegeye D., Crawford T., Chluba J., Remazeilles M., Grainge K.
Physical Review D scimago Q1 wos Q1 , 
2025-03-10,  citations by CoLab: 0 , 
American Physical Society (APS)
Toward a multitracer neutrino mass measurement with line-intensity mapping
Shmueli G., Libanore S., Kovetz E.D.
Physical Review D scimago Q1 wos Q1 , 
2025-03-04,  citations by CoLab: 0 , 
IOP Publishing
The LSPE-Strip pointing reconstruction and Star Tracker
Maris M., Tomasi M., Baratto M., Paonessa F., Franceschet C., Tavagnacco D., Peverini O.A., Villa F., Zannoni M., Bersanelli M., Caccianiga B., Mandelli S., Mennella A., Nati F., Sartor S., et. al.
Journal of Instrumentation scimago Q2 wos Q3 , 
2025-03-01,  citations by CoLab: 0 ,  Abstract  
Abstract This work is part of a series of papers describing in detail the design and characterization of the LSPE-Strip, a microwave telescope operating in the Q- and W-bands which is foreseen to be installed at the Observatorio del Teide in Tenerife. The paper aims to describe the Pointing Reconstruction Model (PRM) and the prototype Star Tracker, which will be mounted on LSPE-Strip. Pointing reconstruction is a crucial step in deriving sky maps of foreground emissions. The PRM will be in charge of integrating the information on the instantaneous attitude provided by the telescope control system, encoded in two control angles, to obtain the actual pointing direction and focal plane orientation of the telescope. The PRM encodes various non-idealities in the telescope setup from eight configuration angles. The Star Tracker, plus the observation of an artificial source installed on a drone and possibly observations of point sources of known positions, will be used to calibrate the configuration angles of the PRM. We study the pointing error produced by incorrectly calibrating configuration angles by comparing surveys with different realizations of systematic pointing errors against the ideal case. In this way, we validated the required ≈ 1 arcmin maximum systematic pointing error in the LSPE-Strip survey as the worst effect of the pointing error, in this case, is two orders of magnitude below the instrumental sensitivity. After a description of the main structure and operations of the Start Tracker, we present the results of a campaign of actual sky observations carried out on a prototype of the Star Tracker aimed at assessing the final Star Tracker accuracy. From the point of view of performance, the Star Tracker prototype fully represents the final Star Tracker, the main differences being related to several implementation details. The results show a Star Tracker RMS accuracy is ≈ 3 arcsec while the systematic error is below 10 arcsec. From those results, we analyzed the problem of reconstructing the PRM configuration angles by simulating a calibration survey. Given the need to intercalibrate the offset of the Start Tracker pointing direction with respect to the focal plane pointing direction, we simulated two possible intercalibration strategies: one by simulating intercalibration with the use of observations of planets, the second by observing a drone carrying an optical beacon and a radio beacon. In the first case, the accuracy is determined by the level of 1/f instrumental plus atmospheric noise, determining the S/N by which the planet can be observed. A very conservative S/N=10 case and a more likely S/N=50 case have been considered, allowing for an intercalibration accuracy respectively of 1 arcmin and 1/3 arcmin. In the second case, the most important source of error is the correct evaluation of the parallaxes between the telescope and the Star Tracker. Our analysis shows that the intercalibration accuracy will be between 0.25 arcmin and 1 arcmin in the worst cases.
IOP Publishing
Stage IV CMB forecasts for warm inflation
dos Santos F.B., Rodrigues G., de Souza R., Alcaniz J.S.
Journal of Cosmology and Astroparticle Physics scimago Q2 wos Q1 , 
2025-03-01,  citations by CoLab: 0 ,  Abstract  
Abstract We report forecast constraints on warm inflation in the light of future cosmic microwave background (CMB) surveys, with data expected to be available in the coming decade. These observations could finally give us the missing information necessary to unveil the production of gravitational waves during inflation, reflected by the detection of a non-zero tensor-to-scalar ratio crucial to the B-mode power spectrum of the CMB. We consider the impact of three future surveys, namely the CMB-S4, Simons Observatory, and the space-borne LiteBIRD, in restricting the parameter space of four typical warm inflationary models in the context of a quartic potential, which is well motivated theoretically. We find that all three surveys significantly improve the models' parameter space, compared to recent results obtained with current Planck+BICEP/Keck Array data. Moreover, the combination of ground-based and space-borne (SO+LiteBIRD and CMB-S4+LiteBIRD) surveys tightens the constraints so that we expect to distinguish even better warm inflation scenarios. This result becomes clear when we compare the models' predictions with a ΛCDM+r forecast, compatible with r = 0, in which one of them already becomes excluded by data.
IOP Publishing
Map-based E/B separation of filtered timestreams using space-based E-mode observations
Zhou Y., Lee A., Chinone Y.
Journal of Cosmology and Astroparticle Physics scimago Q2 wos Q1 , 
2025-03-01,  citations by CoLab: 0 ,  Abstract  
Abstract E to B mixing or "leakage" due to time-ordered data (TOD) filtering has become an important source of sensitivity loss that ground-based cosmic microwave background polarization experiments must address. However, it is a difficult problem for which very few viable solutions exist. In this paper, we expand upon satellite E-mode methods to cover E/B leakage specifically due to TOD filtering. We take a satellite E-mode map and TOD filter it through the ground-based experiment data analysis pipeline, from which we construct a map-space "leakage template" and subtract it from the ground-based experiment map. We evaluate the residual leakage by simulating the satellite E-mode maps with Planck-like and LiteBIRD-like noise levels, and simulate the ground-based experiment with Simons Observatory-like and CMB-S4-like noise levels. The effectiveness of the method is measured in the improvement of the Fisher uncertainty σ(r = 0). We find that our method can reduce σ(r = 0) by ∼ 15–75% depending on the noise levels considered.
IOP Publishing
Stochastic inflation and non-perturbative power spectrum beyond slow roll
Sharma D.
Journal of Cosmology and Astroparticle Physics scimago Q2 wos Q1 , 
2025-03-01,  citations by CoLab: 0 ,  Abstract  
Abstract Stochastic inflation, together with the ΔN formalism, provides a powerful tool for estimating the large-scale behaviour of primordial fluctuations. In this work, we develop a numerical code to capture the non-perturbative statistics of these fluctuations and validate it to obtain the exponential non-Gaussian tail of the curvature perturbations. We present a numerical algorithm to compute the non-perturbative curvature power spectrum and apply it to both slow-roll (SR) and ultra-slow-roll (USR) single-field models of inflation. We accurately generate a non-perturbative scale-invariant power spectrum in the SR scenario. In the USR case, we obtain a peak in the power spectrum that, in the time-independent regime, aligns with the structure of its perturbative counterpart. Additionally, We underscore how the evolving nature of the super-Hubble perturbations in the USR model complicates the numerical computation of the non-perturbative spectrum.
IOP Publishing
Using ΔN eff to constrain preferred axion model dark matter
Cheek A., Min U.
Journal of Cosmology and Astroparticle Physics scimago Q2 wos Q1 , 
2025-03-01,  citations by CoLab: 0 ,  Abstract  
Abstract Preferred axion models are minimal realizations of the Peccei-Quinn solution to the strong CP problem while providing a dark matter candidate. These models invoke new heavy quarks that interact strongly with the Standard Model bringing them into thermal equilibrium in the early Universe. We show that for a number of these models, the heavy quarks will decay after axions have decoupled from the Standard Model thermal bath. As a consequence, any axion products in the decay form a component of dark radiation. This provides the potential to differentiate between preferred axion models through measurements of the number of relativistic degrees of freedom. The most sensitive of which comes from the Planck collaboration's measurements of the Cosmic Microwave Background. We find that existing constraints allow us to rule out regions of parameter space for 40% of the canonical preferred axion models.
IOP Publishing
Unveiling V modes: enhancing CMB sensitivity to BSM physics with a non-ideal half-wave plate
Raffuzzi N., Lembo M., Giardiello S., Gerbino M., Lattanzi M., Natoli P., Pagano L.
Journal of Cosmology and Astroparticle Physics scimago Q2 wos Q1 , 
2025-03-01,  citations by CoLab: 0 ,  Abstract  
Abstract V-mode polarization of the cosmic microwave background is expected to be vanishingly small in the ΛCDM model and, hence, usually ignored. Nonetheless, several astrophysical effects, as well as beyond standard model physics could produce it at a detectable level. A realistic half-wave plate — an optical element commonly used in CMB experiments to modulate the polarized signal — can provide sensitivity to V modes without significantly spoiling that to linear polarization. We assess this sensitivity for some new-generation CMB experiments, such as the LiteBIRD satellite, the ground-based Simons Observatory and a CMB-S4-like experiment. We forecast the efficiency of these experiments to constrain the phenomenology of certain classes of BSM models inducing mixing of linear polarization states and generation of V modes in the CMB. We find that new-generation experiments can improve current limits by 1-to-3 orders of magnitude, depending on the data combination. The inclusion of V-mode information dramatically boosts the sensitivity to these BSM models.
IOP Publishing
The mass effect — variations of the electron mass and their impact on cosmology
Schöneberg N., Vacher L.
Journal of Cosmology and Astroparticle Physics scimago Q2 wos Q1 , 
2025-03-01,  citations by CoLab: 0 ,  Abstract  
Abstract We summarize and explain the current status of time variations of the electron mass in cosmology, showing that such variations allow for significant easing of the Hubble tension, from the current ∼ 5σ significance, down to between 3.4σ and 1.0σ significance, depending on the precise model and data. Electron mass variations are preferred by Cosmic Microwave Background (CMB) data in combination with the latest results on baryonic acoustic oscillations (BAO) and type Ia supernovae at a level of significance between 2σ and 3.6σ depending on the model and the data. This preference for a model involving an electron mass variation is neither tightly constrained from light element abundances generated during big bang nucleosynthesis nor from post-recombination observations using quasars and atomic clocks, though future data is expected to give strong evidence in favor of or against this model.
IOP Publishing
Response of a cold-electron bolometer in a coplanar antenna system
Pimanov D.A., Pankratov A.L., Gordeeva A., Chiginev A., Blagodatkin A., Revin L., Razov S.A., Safonova V.Y., Федотов И., Skorokhodov E., Orlova A., Tatarskiy D.A., Gusev N., Trofimov I., Mumlyakov A., et. al.
Superconductor Science and Technology scimago Q1 wos Q2 , 
2025-03-01,  citations by CoLab: 0 ,  Abstract  
Abstract Cold-electron bolometers have shown suitability for use in modern fundamental physical experiments. In this study, the fabrication and measurements of the samples with cold-electron bolometers integrated into coplanar antennas are performed. The absorber layer was made using combined aluminum-hafnium technology to improve quality of aluminum oxide layer and decrease electron–phonon coupling. The samples of two types were measured in a dilution cryostat at various temperatures from 20 to 300 mK. The first sample with Ti/Au/Pd antenna shows response in the two frequency bands, at 7–9 GHz with bandwidth of about 20%, and also at 14 GHz with 10% bandwidth. The NEP below 10 aW Hz − 1 is reached at 300 mK for 7.7 GHz signal. The second sample with aluminum made antenna shows response in the frequency range 0.5–3 GHz due to the effect of kinetic inductance of superconducting aluminum.
EDP Sciences
QUIJOTE scientific results. XVIII. New constraints on the polarisation of the anomalous microwave emission in bright Galactic regions: ρ Ophiuchi, Perseus, and W43
González-González R., Génova-Santos R.T., Rubiño-Martín J.A., Peel M.W., Guidi F., Lόpez-Caraballo C.H., Fernández-Torreiro M., Rebolo R., Hernandez-Monteagudo C., Adak D., Artal E., Ashdown M., Barreiro R.B., Casas F.J., Cepeda-Arroita R., et. al.
Astronomy and Astrophysics scimago Q1 wos Q1 , 
2025-03-01,  citations by CoLab: 0 ,  Abstract  
This work focuses on the study of the anomalous microwave emission (AME), an important emission mechanism between 10 and 60 GHz whose polarisation properties are not yet fully understood and is therefore a potential contaminant for future cosmic microwave background (CMB) polarisation observations. We used new QUIJOTE-MFI maps at 11, 13, 17, and 19 GHz obtained from the combination of the public wide survey data and additional 1800 h of dedicated raster scan observations together with other public ancillary data, including WMAP and Planck, to study the polarisation properties of the AME in three Galactic regions: ρ Ophiuchi, Perseus, and W43. We obtained the spectral energy distributions (SEDs) of the three regions over the frequency range 0.4–3000 GHz in intensity and polarisation. The intensity SEDs are well described by a combination of free-free emission, thermal dust, AME, and CMB anisotropies. In polarisation, we extracted the flux densities using all available data between 11 and 353 GHz. We implemented an improved intensity-to-polarisation leakage correction that allowed reliable polarisation constraints well below the 1% level from Planck-LFI data to be derived for the first time. A frequency stacking of maps in the range 10–60 GHz allowed us to reduce the statistical noise and to push the upper limits on the AME polarisation level. We obtained upper limits on the AME polarisation fraction of the order ≲1% (95% confidence level) for the three regions. In particular, we obtained ΠAME < 1.0% (at 28.4 GHz), ΠAME < 0.9% (at 28.4 GHz), and ΠAME < 0.28% (at 33 GHz) in ρ Ophiuchi, Perseus, and W43, respectively. At the QUIJOTE 17 GHz frequency band, we found ΠAME < 5.0% for ρ Ophiuchi, ΠAME < 3.4% for Perseus, and ΠAME < 0.85% for W43. We note that for the ρ Ophiuchi molecular cloud, the new QUIJOTE-MFI data allowed us to set the first constraints on the AME polarisation in the range 10–20 GHz. Our final upper limits derived using the stacking procedure are ΠAME < 0.58% for ρ Ophiuchi, ΠAME < 0.67% for Perseus, and ΠAME < 0.31% for W43. Altogether, these are the most stringent constraints to date on the AME polarisation fraction of these three star-forming regions.
American Astronomical Society
A Measurement of Atmospheric Circular Polarization with POLARBEAR
Fujino T., Takakura S., Arani S.S., Barron D., Baccigalupi C., Chinone Y., Errard J., Fabbian G., Feng C., Halverson N.W., Hasegawa M., Hazumi M., Jeong O., Kaneko D., Keating B., et. al.
Astrophysical Journal scimago Q1 wos Q1 Open Access , 
2025-02-21,  citations by CoLab: 0 ,  Abstract  
Abstract At millimeter wavelengths, the atmospheric emission is circularly polarized owing to the Zeeman splitting of molecular oxygen by the Earth's magnetic field. We report a measurement of the signal in the 150 GHz band using 3 yr of observational data with the Polarbear project. Nonidealities of a continuously rotating half-wave plate (HWP) partially convert circularly polarized light to linearly polarized light. While Polarbear detectors are sensitive to linear polarization, this effect makes them sensitive to circular polarization. Although this was not the intended use, we utilized this conversion to measure circular polarization. We reconstruct the azimuthal gradient of the circular polarization signal and measure its dependency from the scanning direction and the detector bandpass. We compare the signal with a simulation based on atmospheric emission theory, the detector bandpass, and the HWP leakage spectrum model. We find the ratio of the observed azimuthal slope to the simulated slope is 0.92 ± 0.01(stat) ± 0.07(sys). This ratio corresponds to a brightness temperature of 3.8 mK at the effective band center of 121.8 GHz and bandwidth of 3.5 GHz estimated from representative detector bandpass and the spectrum of Zeeman emission. This result validates our understanding of the instrument and reinforces the feasibility of measuring the circular polarization using the imperfection of continuously rotating HWP. Continuously rotating HWP is popular in ongoing and future cosmic microwave background experiments to modulate the polarized signal. This work shows a method for signal extraction and leakage subtraction that can help measure circular polarization in such experiments.
American Physical Society (APS)
Validating a main beam treatment of parametric, pixel-based component separation in the context of CMB observations
Rizzieri A., Errard J., Stompor R.
Physical Review D scimago Q1 wos Q1 , 
2025-02-06,  citations by CoLab: 0 , 

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Journal of Cosmology and Astroparticle Physics
Journal of Cosmology and Astroparticle Physics, 72, 40%
Physical Review D
Physical Review D, 32, 17.78%
Monthly Notices of the Royal Astronomical Society
Monthly Notices of the Royal Astronomical Society, 8, 4.44%
Astronomy and Astrophysics
Astronomy and Astrophysics, 8, 4.44%
Physical Review Letters
Physical Review Letters, 7, 3.89%
Journal of Low Temperature Physics
Journal of Low Temperature Physics, 6, 3.33%
Astrophysical Journal
Astrophysical Journal, 5, 2.78%
Physics Letters, Section B: Nuclear, Elementary Particle and High-Energy Physics
Physics Letters, Section B: Nuclear, Elementary Particle and High-Energy Physics, 3, 1.67%
Astrophysical Journal, Supplement Series
Astrophysical Journal, Supplement Series, 2, 1.11%
Monthly Notices of the Royal Astronomical Society: Letters
Monthly Notices of the Royal Astronomical Society: Letters, 2, 1.11%
Physics of the Dark Universe
Physics of the Dark Universe, 2, 1.11%
Journal of Astronomical Telescopes, Instruments, and Systems
Journal of Astronomical Telescopes, Instruments, and Systems, 1, 0.56%
SciPost Physics, 1, 0.56%
Journal of Applied Physics
Journal of Applied Physics, 1, 0.56%
Inventions
Inventions, 1, 0.56%
Beilstein Journal of Nanotechnology
Beilstein Journal of Nanotechnology, 1, 0.56%
Physical Review Research
Physical Review Research, 1, 0.56%
Progress of Theoretical and Experimental Physics
Progress of Theoretical and Experimental Physics, 1, 0.56%
Applied Thermal Engineering
Applied Thermal Engineering, 1, 0.56%
European Physical Journal C
European Physical Journal C, 1, 0.56%
Journal of High Energy Astrophysics
Journal of High Energy Astrophysics, 1, 0.56%
Applied Optics
Applied Optics, 1, 0.56%
Journal of Instrumentation
Journal of Instrumentation, 1, 0.56%
Publications of the Astronomical Society of the Pacific
Publications of the Astronomical Society of the Pacific, 1, 0.56%
Physical Review Applied
Physical Review Applied, 1, 0.56%
Chinese Physics C
Chinese Physics C, 1, 0.56%
Superconductor Science and Technology
Superconductor Science and Technology, 1, 0.56%
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Publishers

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IOP Publishing
IOP Publishing, 76, 42.22%
American Physical Society (APS)
American Physical Society (APS), 41, 22.78%
SPIE-Intl Soc Optical Eng
SPIE-Intl Soc Optical Eng, 18, 10%
Oxford University Press
Oxford University Press, 11, 6.11%
EDP Sciences
EDP Sciences, 8, 4.44%
American Astronomical Society
American Astronomical Society, 7, 3.89%
Elsevier
Elsevier, 7, 3.89%
Springer Nature
Springer Nature, 7, 3.89%
Stichting SciPost, 1, 0.56%
AIP Publishing
AIP Publishing, 1, 0.56%
MDPI
MDPI, 1, 0.56%
Beilstein-Institut
Beilstein-Institut, 1, 0.56%
Optica Publishing Group
Optica Publishing Group, 1, 0.56%
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