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1. 3D atomic structure from a single XFEL pulse

Author

Bortel, G., Tegze, M., Sikorski, M., Bean, R., Bielecki, J., Kim, C., Koliyadu, J., Koua, F., Ramilli, M., Round, A., Sato, T., Zabelskii, D., and Faigel, G.

Subjects
Condensed Matter - Materials Science
Abstract

X-ray Free Electron Lasers (XFEL) are the most advanced pulsed x-ray sources. Their extraordinary pulse parameters promise unique applications. Indeed, several new methods have been developed at XFEL-s. However, no methods are known, which would allow ab initio atomic level structure determination using only a single XFEL pulse. Here, we present experimental results, demonstrating the determination of the 3D atomic structure from data obtained during a single 25 fs XFEL pulse. Parallel measurement of hundreds of Bragg reflections was done by collecting Kossel line patterns of GaAs and GaP. With these measurements, we reached the ultimate temporal limit of the x-ray structure solution possible today. These measurements open the way for studying non-repeatable fast processes and structural transformations in crystals for example measuring the atomic structure of matter at extremely non-ambient conditions or transient structures formed in irreversible physical, chemical, or biological processes. It would also facilitate time resolved pump-probe structural studies making them significantly shorter than traditional serial crystallography., Comment: 16 pages of manuscript followed by 15 pages of supplementary information

Published
2023

2. The Atacama Cosmology Telescope: Probing the baryon content of SDSS DR15 galaxies with the thermal and kinematic Sunyaev-Zel’dovich effects

Author

Vavagiakis, EM, Gallardo, PA, Calafut, V, Amodeo, S, Aiola, S, Austermann, JE, Battaglia, N, Battistelli, ES, Beall, JA, Bean, R, Bond, JR, Calabrese, E, Choi, SK, Cothard, NF, Devlin, MJ, Duell, CJ, Duff, SM, Duivenvoorden, AJ, Dunkley, J, Dunner, R, Ferraro, S, Guan, Y, Hill, JC, Hilton, GC, Hilton, M, Hložek, R, Huber, ZB, Hubmayr, J, Huffenberger, KM, Hughes, JP, Koopman, BJ, Kosowsky, A, Li, Y, Lokken, M, Madhavacheril, M, McMahon, J, Moodley, K, Naess, S, Nati, F, Newburgh, LB, Niemack, MD, Page, LA, Partridge, B, Schaan, E, Schillaci, A, Sifón, C, Spergel, DN, Staggs, ST, Ullom, JN, Vale, LR, Van Engelen, A, Van Lanen, J, Wollack, EJ, and Xu, Z

Subjects
Astronomical Sciences, Physical Sciences
Abstract

We present measurements of the average thermal Sunyaev Zel’dovich (tSZ) effect from optically selected galaxy groups and clusters at high signal-to-noise (up to ) and estimate their baryon content within a radius aperture. Sources from the Sloan Digital Sky Survey Baryon Oscillation Spectroscopic Survey DR15 catalog overlap with 3,700 sq deg of sky observed by the Atacama Cosmology Telescope (ACT) from 2008 to 2018 at 150 and 98 GHz (ACT DR5), and 2,089 sq deg of internal linear combination component-separated maps combining ACT and Planck data (ACT DR4). The corresponding optical depths , which depend on the baryon content of the halos, are estimated using results from cosmological hydrodynamic simulations assuming an active galactic nuclei feedback radiative cooling model. We estimate the mean mass of the halos in multiple luminosity bins, and compare the tSZ-based estimates to theoretical predictions of the baryon content for a Navarro-Frenk-White profile. We do the same for estimates extracted from fits to pairwise baryon momentum measurements of the kinematic Sunyaev-Zel’dovich effect (kSZ) for the same dataset obtained in a companion paper. We find that the estimates from the tSZ measurements in this work and the kSZ measurements in the companion paper agree within for two out of the three disjoint luminosity bins studied, while they differ by in the highest luminosity bin. The optical depth estimates account for one-third to all of the theoretically predicted baryon content in the halos across luminosity bins. Potential systematic uncertainties are discussed. The tSZ and kSZ measurements provide a step toward empirical Compton- relationships to provide new tests of cluster formation and evolution models.

Published
2021

3. The Atacama Cosmology Telescope: Detection of the pairwise kinematic Sunyaev-Zel’dovich effect with SDSS DR15 galaxies

Author

Calafut, V, Gallardo, PA, Vavagiakis, EM, Amodeo, S, Aiola, S, Austermann, JE, Battaglia, N, Battistelli, ES, Beall, JA, Bean, R, Bond, JR, Calabrese, E, Choi, SK, Cothard, NF, Devlin, MJ, Duell, CJ, Duff, SM, Duivenvoorden, AJ, Dunkley, J, Dunner, R, Ferraro, S, Guan, Y, Hill, JC, Hilton, GC, Hilton, M, Hložek, R, Huber, ZB, Hubmayr, J, Huffenberger, KM, Hughes, JP, Koopman, BJ, Kosowsky, A, Li, Y, Lokken, M, Madhavacheril, M, McMahon, J, Moodley, K, Naess, S, Nati, F, Newburgh, LB, Niemack, MD, Page, LA, Partridge, B, Schaan, E, Schillaci, A, Sifón, C, Spergel, DN, Staggs, ST, Ullom, JN, Vale, LR, Van Engelen, A, Van Lanen, J, Wollack, EJ, and Xu, Z

Subjects
Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Quantum Physics, Nuclear & Particles Physics
Abstract

We present a detection of the pairwise kinematic Sunyaev-Zeldovich (kSZ) effect using Atacama Cosmology Telescope (ACT) and Planck CMB observations in combination with Luminous Red Galaxy samples from the Sloan Digital Sky Survey (SDSS) DR15 catalog. Results are obtained using three ACT CMB maps: co-added 150 and 98 GHz maps, combining observations from 2008-2018 (ACT DR5), which overlap with SDSS DR15 over 3,700 sq. deg., and a component-separated map using night-time only observations from 2014-2015 (ACT DR4), overlapping with SDSS DR15 over 2,089 sq. deg. Comparisons of the results from these three maps provide consistency checks in relation to potential frequency-dependent foreground contamination. A total of 343,647 galaxies are used as tracers to identify and locate galaxy groups and clusters from which the kSZ signal is extracted using aperture photometry. We consider the impact of various aperture photometry assumptions and covariance estimation methods on the signal extraction. Theoretical predictions of the pairwise velocities are used to obtain best-fit, mass-averaged, optical depth estimates for each of five luminosity-selected tracer samples. A comparison of the kSZ-derived optical depth measurements obtained here to those derived from the thermal SZ effect for the same sample is presented in a companion paper.

Published
2021

4. Atacama Cosmology Telescope: Modeling the gas thermodynamics in BOSS CMASS galaxies from kinematic and thermal Sunyaev-Zel'dovich measurements

Author

Amodeo, S, Battaglia, N, Schaan, E, Ferraro, S, Moser, E, Aiola, S, Austermann, JE, Beall, JA, Bean, R, Becker, DT, Bond, RJ, Calabrese, E, Calafut, V, Choi, SK, Denison, EV, Devlin, M, Duff, SM, Duivenvoorden, AJ, Dunkley, J, Dünner, R, Gallardo, PA, Hall, KR, Han, D, Hill, JC, Hilton, GC, Hilton, M, HloŽek, R, Hubmayr, J, Huffenberger, KM, Hughes, JP, Koopman, BJ, Macinnis, A, McMahon, J, Madhavacheril, MS, Moodley, K, Mroczkowski, T, Naess, S, Nati, F, Newburgh, LB, Niemack, MD, Page, LA, Partridge, B, Schillaci, A, Sehgal, N, Sifón, C, Spergel, DN, Staggs, S, Storer, ER, Ullom, JN, Vale, LR, Van Engelen, A, Van Lanen, J, Vavagiakis, EM, Wollack, EJ, and Xu, Z

Subjects
astro-ph.CO, astro-ph.GA
Abstract

The thermal and kinematic Sunyaev-Zel'dovich effects (tSZ, kSZ) probe the thermodynamic properties of the circumgalactic and intracluster medium (CGM and ICM) of galaxies, groups, and clusters, since they are proportional, respectively, to the integrated electron pressure and momentum along the line of sight. We present constraints on the gas thermodynamics of CMASS (constant stellar mass) galaxies in the Baryon Oscillation Spectroscopic Survey using new measurements of the kSZ and tSZ signals obtained in a companion paper [Schaan et al.]. Combining kSZ and tSZ measurements, we measure within our model the amplitude of energy injection ϵM⋆c2, where M⋆ is the stellar mass, to be ϵ=(40±9)×10-6, and the amplitude of the nonthermal pressure profile to be αNth

Published
2021

5. Atacama Cosmology Telescope: Combined kinematic and thermal Sunyaev-Zel'dovich measurements from BOSS CMASS and LOWZ halos

Author

Schaan, E, Ferraro, S, Amodeo, S, Battaglia, N, Aiola, S, Austermann, JE, Beall, JA, Bean, R, Becker, DT, Bond, RJ, Calabrese, E, Calafut, V, Choi, SK, Denison, EV, Devlin, MJ, Duff, SM, Duivenvoorden, AJ, Dunkley, J, Dünner, R, Gallardo, PA, Guan, Y, Han, D, Hill, JC, Hilton, GC, Hilton, M, HloŽek, R, Hubmayr, J, Huffenberger, KM, Hughes, JP, Koopman, BJ, Macinnis, A, McMahon, J, Madhavacheril, MS, Moodley, K, Mroczkowski, T, Naess, S, Nati, F, Newburgh, LB, Niemack, MD, Page, LA, Partridge, B, Salatino, M, Sehgal, N, Schillaci, A, Sifón, C, Smith, KM, Spergel, DN, Staggs, S, Storer, ER, Trac, H, Ullom, JN, Van Lanen, J, Vale, LR, Van Engelen, A, Magaña, MV, Vavagiakis, EM, Wollack, EJ, and Xu, Z

Subjects
astro-ph.CO, astro-ph.GA
Abstract

The scattering of cosmic microwave background (CMB) photons off the free-electron gas in galaxies and clusters leaves detectable imprints on high resolution CMB maps: the thermal and kinematic Sunyaev-Zel'dovich effects (tSZ and kSZ respectively). We use combined microwave maps from the Atacama Cosmology Telescope DR5 and Planck in combination with the CMASS (mean redshift ⟨z

Published
2021

6. Megahertz single-particle imaging at the European XFEL

Author

Sobolev, E, Zolotarev, S, Giewekemeyer, K, Bielecki, J, Okamoto, K, Reddy, HKN, Andreasson, J, Ayyer, K, Barak, I, Bari, S, Barty, A, Bean, R, Bobkov, S, Chapman, HN, Chojnowski, G, Daurer, BJ, Dörner, K, Ekeberg, T, Flückiger, L, Galzitskaya, O, Gelisio, L, Hauf, S, Hogue, BG, Horke, DA, Hosseinizadeh, A, Ilyin, V, Jung, C, Kim, C, Kim, Y, Kirian, RA, Kirkwood, H, Kulyk, O, Küpper, J, Letrun, R, Loh, ND, Lorenzen, K, Messerschmidt, M, Mühlig, K, Ourmazd, A, Raab, N, Rode, AV, Rose, M, Round, A, Sato, T, Schubert, R, Schwander, P, Sellberg, JA, Sikorski, M, Silenzi, A, Song, C, Spence, JCH, Stern, S, Sztuk-Dambietz, J, Teslyuk, A, Timneanu, N, Trebbin, M, Uetrecht, C, Weinhausen, B, Williams, GJ, Xavier, PL, Xu, C, Vartanyants, IA, Lamzin, VS, Mancuso, A, and Maia, FRNC

Abstract

The emergence of high repetition-rate X-ray free-electron lasers (XFELs) powered by superconducting accelerator technology enables the measurement of significantly more experimental data per day than was previously possible. The European XFEL is expected to provide 27,000 pulses per second, over two orders of magnitude more than any other XFEL. The increased pulse rate is a key enabling factor for single-particle X-ray diffractive imaging, which relies on averaging the weak diffraction signal from single biological particles. Taking full advantage of this new capability requires that all experimental steps, from sample preparation and delivery to the acquisition of diffraction patterns, are compatible with the increased pulse repetition rate. Here, we show that single-particle imaging can be performed using X-ray pulses at megahertz repetition rates. The results obtained pave the way towards exploiting high repetition-rate X-ray free-electron lasers for single-particle imaging at their full repetition rate.

Published
2020

7. The Atacama Cosmology Telescope: DR4 maps and cosmological parameters

Author

Aiola, S, Calabrese, E, Maurin, L, Naess, S, Schmitt, BL, Abitbol, MH, Addison, GE, Ade, PAR, Alonso, D, Amiri, M, Amodeo, S, Angile, E, Austermann, JE, Baildon, T, Battaglia, N, Beall, JA, Bean, R, Becker, DT, Richard Bond, J, Bruno, SM, Calafut, V, Campusano, LE, Carrero, F, Chesmore, GE, Cho, HM, Choi, SK, Clark, SE, Cothard, NF, Crichton, D, Crowley, KT, Darwish, O, Datta, R, Denison, EV, Devlin, MJ, Duell, CJ, Duff, SM, Duivenvoorden, AJ, Dunkley, J, Dünner, R, Essinger-Hileman, T, Fankhanel, M, Ferraro, S, Fox, AE, Fuzia, B, Gallardo, PA, Gluscevic, V, Golec, JE, Grace, E, Gralla, M, Guan, Y, Hall, K, Halpern, M, Han, D, Hargrave, P, Hasselfield, M, Helton, JM, Henderson, S, Hensley, B, Colin Hill, J, Hilton, GC, Hilton, M, Hincks, AD, Hložek, R, Ho, SPP, Hubmayr, J, Huffenberger, KM, Hughes, JP, Infante, L, Irwin, K, Jackson, R, Klein, J, Knowles, K, Koopman, B, Kosowsky, A, Lakey, V, Li, D, Li, Y, Li, Z, Lokken, M, Louis, T, Lungu, M, MacInnis, A, Madhavacheril, M, Maldonado, F, Mallaby-Kay, M, Marsden, D, McMahon, J, Menanteau, F, Moodley, K, Morton, T, Namikawa, T, Nati, F, Newburgh, L, Nibarger, JP, Nicola, A, Niemack, MD, Nolta, MR, Orlowski-Sherer, J, Page, LA, and Pappas, CG

Subjects
CMBR experiments, CMBR polarisation, cosmological parameters from CMBR, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Nuclear & Particles Physics, Atomic, Molecular, Nuclear, Particle and Plasma Physics
Abstract

We present new arcminute-resolution maps of the Cosmic Microwave Background temperature and polarization anisotropy from the Atacama Cosmology Telescope, using data taken from 2013–2016 at 98 and 150 GHz. The maps cover more than 17,000 deg2, the deepest 600 deg2 with noise levels below 10µK-arcmin. We use the power spectrum derived from almost 6,000 deg2 of these maps to constrain cosmology. The ACT data enable a measurement of the angular scale of features in both the divergence-like polarization and the temperature anisotropy, tracing both the velocity and density at last-scattering. From these one can derive the distance to the last-scattering surface and thus infer the local expansion rate, H0. By combining ACT data with large-scale information from WMAP we measure H0 = 67.6±1.1 km/s/Mpc, at 68% confidence, in excellent agreement with the independently-measured Planck satellite estimate (from ACT alone we find H0 = 67.9 ± 1.5 km/s/Mpc). The ΛCDM model provides a good fit to the ACT data, and we find no evidence for deviations: both the spatial curvature, and the departure from the standard lensing signal in the spectrum, are zero to within 1σ; the number of relativistic species, the primordial Helium fraction, and the running of the spectral index are consistent with ΛCDM predictions to within 1.5–2.2σ. We compare ACT, WMAP, and Planck at the parameter level and find good consistency; we investigate how the constraints on the correlated spectral index and baryon density parameters readjust when adding CMB large-scale information that ACT does not measure. The DR4 products presented here will be publicly released on the NASA Legacy Archive for Microwave Background Data Analysis.

Published
2020

8. The atacama cosmology telescope: A measurement of the cosmic microwave background power spectra at 98 and 150 GHz

Author

Choi, SK, Hasselfield, M, Ho, SPP, Koopman, B, Lungu, M, Abitbol, MH, Addison, GE, Ade, PAR, Aiola, S, Alonso, D, Amiri, M, Amodeo, S, Angile, E, Austermann, JE, Baildon, T, Battaglia, N, Beall, JA, Bean, R, Becker, DT, Richard Bond, J, Bruno, SM, Calabrese, E, Calafut, V, Campusano, LE, Carrero, F, Chesmore, GE, Cho, HM, Clark, SE, Cothard, NF, Crichton, D, Crowley, KT, Darwish, O, Datta, R, Denison, EV, Devlin, MJ, Duell, CJ, Duff, SM, Duivenvoorden, AJ, Dunkley, J, Dünner, R, Essinger-Hileman, T, Fankhanel, M, Ferraro, S, Fox, AE, Fuzia, B, Gallardo, PA, Gluscevic, V, Golec, JE, Grace, E, Gralla, M, Guan, Y, Hall, K, Halpern, M, Han, D, Hargrave, P, Henderson, S, Hensley, B, Colin Hill, J, Hilton, GC, Hilton, M, Hincks, AD, Hložek, R, Hubmayr, J, Huffenberger, KM, Hughes, JP, Infante, L, Irwin, K, Jackson, R, Klein, J, Knowles, K, Kosowsky, A, Lakey, V, Li, D, Li, Y, Li, Z, Lokken, M, Louis, T, MacInnis, A, Madhavacheril, M, Maldonado, F, Mallaby-Kay, M, Marsden, D, Maurin, L, McMahon, J, Menanteau, F, Moodley, K, Morton, T, Naess, S, Namikawa, T, Nati, F, Newburgh, L, Nibarger, JP, Nicola, A, Niemack, MD, Nolta, MR, Orlowski-Sherer, J, Page, LA, Pappas, CG, Partridge, B, and Phakathi, P

Subjects
CMBR experiments, CMBR polarisation, cosmological parameters from CMBR, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Nuclear & Particles Physics, Atomic, Molecular, Nuclear, Particle and Plasma Physics
Abstract

We present the temperature and polarization angular power spectra of the CMB measured by the Atacama Cosmology Telescope (ACT) from 5400 deg2 of the 2013–2016 survey, which covers >15000 deg2 at 98 and 150 GHz. For this analysis we adopt a blinding strategy to help avoid confirmation bias and, related to this, show numerous checks for systematic error done before unblinding. Using the likelihood for the cosmological analysis we constrain secondary sources of anisotropy and foreground emission, and derive a “CMB-only” spectrum that extends to ` = 4000. At large angular scales, foreground emission at 150 GHz is ∼1% of TT and EE within our selected regions and consistent with that found by Planck. Using the same likelihood, we obtain the cosmological parameters for ΛCDM for the ACT data alone with a prior on the optical depth of τ = 0.065 ± 0.015. ΛCDM is a good fit. The best-fit model has a reduced χ2 of 1.07 (PTE = 0.07) with H0 = 67.9 ± 1.5 km/s/Mpc. We show that the lensing BB signal is consistent with ΛCDM and limit the celestial EB polarization angle to ψP = −0.07◦ ±0.09◦. We directly cross correlate ACT with Planck and observe generally good agreement but with some discrepancies in TE. All data on which this analysis is based will be publicly released.

Published
2020

9. Atacama Cosmology Telescope: Component-separated maps of CMB temperature and the thermal Sunyaev-Zel'dovich effect

Author

Madhavacheril, MS, Hill, JC, Næss, S, Addison, GE, Aiola, S, Baildon, T, Battaglia, N, Bean, R, Bond, JR, Calabrese, E, Calafut, V, Choi, SK, Darwish, O, Datta, R, Devlin, MJ, Dunkley, J, Dünner, R, Ferraro, S, Gallardo, PA, Gluscevic, V, Halpern, M, Han, D, Hasselfield, M, Hilton, M, Hincks, AD, HloŽek, R, Ho, SPP, Huffenberger, KM, Hughes, JP, Koopman, BJ, Kosowsky, A, Lokken, M, Louis, T, Lungu, M, Macinnis, A, Maurin, L, McMahon, JJ, Moodley, K, Nati, F, Niemack, MD, Page, LA, Partridge, B, Robertson, N, Sehgal, N, Schaan, E, Schillaci, A, Sherwin, BD, Sifón, C, Simon, SM, Spergel, DN, Staggs, ST, Storer, ER, Van Engelen, A, Vavagiakis, EM, Wollack, EJ, and Xu, Z

Subjects
astro-ph.CO, astro-ph.GA
Abstract

Optimal analyses of many signals in the cosmic microwave background (CMB) require map-level extraction of individual components in the microwave sky, rather than measurements at the power spectrum level alone. To date, nearly all map-level component separation in CMB analyses has been performed exclusively using satellite data. In this paper, we implement a component separation method based on the internal linear combination (ILC) approach which we have designed to optimally account for the anisotropic noise (in the 2D Fourier domain) often found in ground-based CMB experiments. Using this method, we combine multifrequency data from the Planck satellite and the Atacama Cosmology Telescope Polarimeter (ACTPol) to construct the first wide-area (≈2100 sq. deg.), arcminute-resolution component-separated maps of the CMB temperature anisotropy and the thermal Sunyaev-Zel'dovich (tSZ) effect sourced by the inverse-Compton scattering of CMB photons off hot, ionized gas. Our ILC pipeline allows for explicit deprojection of various contaminating signals, including a modified blackbody approximation of the cosmic infrared background (CIB) spectral energy distribution. The cleaned CMB maps will be a useful resource for CMB lensing reconstruction, kinematic SZ cross-correlations, and primordial non-Gaussianity studies. The tSZ maps will be used to study the pressure profiles of galaxies, groups, and clusters through cross-correlations with halo catalogs, with dust contamination controlled via CIB deprojection. The data products described in this paper are available on LAMBDA.

Published
2020

11. The Atacama Cosmology Telescope: DR6 Gravitational Lensing Map and Cosmological Parameters

Author

Madhavacheril, M, Qu, F, Sherwin, B, Maccrann, N, Li, Y, Abril-Cabezas, I, Ade, P, Aiola, S, Alford, T, Amiri, M, Amodeo, S, An, R, Atkins, Z, Austermann, J, Battaglia, N, Battistelli, E, Beall, J, Bean, R, Beringue, B, Bhandarkar, T, Biermann, E, Bolliet, B, Bond, J, Cai, H, Calabrese, E, Calafut, V, Capalbo, V, Carrero, F, Challinor, A, Chesmore, G, Cho, H, Choi, S, Clark, S, Rosado, R, Cothard, N, Coughlin, K, Coulton, W, Crowley, K, Dalal, R, Darwish, O, Devlin, M, Dicker, S, Doze, P, Duell, C, Duff, S, Duivenvoorden, A, Dunkley, J, Dunner, R, Fanfani, V, Fankhanel, M, Farren, G, Ferraro, S, Freundt, R, Fuzia, B, Gallardo, P, Garrido, X, Givans, J, Gluscevic, V, Golec, J, Guan, Y, Hall, K, Halpern, M, Han, D, Harrison, I, Hasselfield, M, Healy, E, Henderson, S, Hensley, B, Hervias-Caimapo, C, Hill, J, Hilton, G, Hilton, M, Hincks, A, Hlozek, R, Ho, S, Huber, Z, Hubmayr, J, Huffenberger, K, Hughes, J, Irwin, K, Isopi, G, Jense, H, Keller, B, Kim, J, Knowles, K, Koopman, B, Kosowsky, A, Kramer, D, Kusiak, A, La Posta, A, Lague, A, Lakey, V, Lee, E, Li, Z, Limon, M, Lokken, M, Louis, T, Lungu, M, Macinnis, A, Maldonado, D, Maldonado, F, Mallaby-Kay, M, Marques, G, Mcmahon, J, Mehta, Y, Menanteau, F, Moodley, K, Morris, T, Mroczkowski, T, Naess, S, Namikawa, T, Nati, F, Newburgh, L, Nicola, A, Niemack, M, Nolta, M, Orlowski-Scherer, J, Page, L, Pandey, S, Partridge, B, Prince, H, Puddu, R, Radiconi, F, Robertson, N, Rojas, F, Sakuma, T, Salatino, M, Schaan, E, Schmitt, B, Sehgal, N, Shaikh, S, Sierra, C, Sievers, J, Sifon, C, Simon, S, Sonka, R, Spergel, D, Staggs, S, Storer, E, Switzer, E, Tampier, N, Thornton, R, Trac, H, Treu, J, Tucker, C, Ullom, J, Vale, L, Van Engelen, A, Van Lanen, J, van Marrewijk, J, Vargas, C, Vavagiakis, E, Wagoner, K, Wang, Y, Wenzl, L, Wollack, E, Xu, Z, Zago, F, Zheng, K, Madhavacheril M. S., Qu F. J., Sherwin B. D., MacCrann N., Li Y., Abril-Cabezas I., Ade P. A. R., Aiola S., Alford T., Amiri M., Amodeo S., An R., Atkins Z., Austermann J. E., Battaglia N., Battistelli E. S., Beall J. A., Bean R., Beringue B., Bhandarkar T., Biermann E., Bolliet B., Bond J. R., Cai H., Calabrese E., Calafut V., Capalbo V., Carrero F., Challinor A., Chesmore G. E., Cho H. -M., Choi S. K., Clark S. E., Rosado R. C., Cothard N. F., Coughlin K., Coulton W., Crowley K. T., Dalal R., Darwish O., Devlin M. J., Dicker S., Doze P., Duell C. J., Duff S. M., Duivenvoorden A. J., Dunkley J., Dunner R., Fanfani V., Fankhanel M., Farren G., Ferraro S., Freundt R., Fuzia B., Gallardo P. A., Garrido X., Givans J., Gluscevic V., Golec J. E., Guan Y., Hall K. R., Halpern M., Han D., Harrison I., Hasselfield M., Healy E., Henderson S., Hensley B., Hervias-Caimapo C., Hill J. C., Hilton G. C., Hilton M., Hincks A. D., Hlozek R., Ho S. P., Huber Z. B., Hubmayr J., Huffenberger K. M., Hughes J. P., Irwin K., Isopi G., Jense H. T., Keller B., Kim J., Knowles K., Koopman B. J., Kosowsky A., Kramer D., Kusiak A., La Posta A., Lague A., Lakey V., Lee E., Li Z., Limon M., Lokken M., Louis T., Lungu M., MacInnis A., Maldonado D., Maldonado F., Mallaby-Kay M., Marques G. A., McMahon J., Mehta Y., Menanteau F., Moodley K., Morris T. W., Mroczkowski T., Naess S., Namikawa T., Nati F., Newburgh L., Nicola A., Niemack M. D., Nolta M. R., Orlowski-Scherer J., Page L. A., Pandey S., Partridge B., Prince H., Puddu R., Radiconi F., Robertson N., Rojas F., Sakuma T., Salatino M., Schaan E., Schmitt B. L., Sehgal N., Shaikh S., Sierra C., Sievers J., Sifon C., Simon S., Sonka R., Spergel D. N., Staggs S. T., Storer E., Switzer E. R., Tampier N., Thornton R., Trac H., Treu J., Tucker C., Ullom J., Vale L. R., Van Engelen A., Van Lanen J., van Marrewijk J., Vargas C., Vavagiakis E. M., Wagoner K., Wang Y., Wenzl L., Wollack E. J., Xu Z., Zago F., Zheng K., Madhavacheril, M, Qu, F, Sherwin, B, Maccrann, N, Li, Y, Abril-Cabezas, I, Ade, P, Aiola, S, Alford, T, Amiri, M, Amodeo, S, An, R, Atkins, Z, Austermann, J, Battaglia, N, Battistelli, E, Beall, J, Bean, R, Beringue, B, Bhandarkar, T, Biermann, E, Bolliet, B, Bond, J, Cai, H, Calabrese, E, Calafut, V, Capalbo, V, Carrero, F, Challinor, A, Chesmore, G, Cho, H, Choi, S, Clark, S, Rosado, R, Cothard, N, Coughlin, K, Coulton, W, Crowley, K, Dalal, R, Darwish, O, Devlin, M, Dicker, S, Doze, P, Duell, C, Duff, S, Duivenvoorden, A, Dunkley, J, Dunner, R, Fanfani, V, Fankhanel, M, Farren, G, Ferraro, S, Freundt, R, Fuzia, B, Gallardo, P, Garrido, X, Givans, J, Gluscevic, V, Golec, J, Guan, Y, Hall, K, Halpern, M, Han, D, Harrison, I, Hasselfield, M, Healy, E, Henderson, S, Hensley, B, Hervias-Caimapo, C, Hill, J, Hilton, G, Hilton, M, Hincks, A, Hlozek, R, Ho, S, Huber, Z, Hubmayr, J, Huffenberger, K, Hughes, J, Irwin, K, Isopi, G, Jense, H, Keller, B, Kim, J, Knowles, K, Koopman, B, Kosowsky, A, Kramer, D, Kusiak, A, La Posta, A, Lague, A, Lakey, V, Lee, E, Li, Z, Limon, M, Lokken, M, Louis, T, Lungu, M, Macinnis, A, Maldonado, D, Maldonado, F, Mallaby-Kay, M, Marques, G, Mcmahon, J, Mehta, Y, Menanteau, F, Moodley, K, Morris, T, Mroczkowski, T, Naess, S, Namikawa, T, Nati, F, Newburgh, L, Nicola, A, Niemack, M, Nolta, M, Orlowski-Scherer, J, Page, L, Pandey, S, Partridge, B, Prince, H, Puddu, R, Radiconi, F, Robertson, N, Rojas, F, Sakuma, T, Salatino, M, Schaan, E, Schmitt, B, Sehgal, N, Shaikh, S, Sierra, C, Sievers, J, Sifon, C, Simon, S, Sonka, R, Spergel, D, Staggs, S, Storer, E, Switzer, E, Tampier, N, Thornton, R, Trac, H, Treu, J, Tucker, C, Ullom, J, Vale, L, Van Engelen, A, Van Lanen, J, van Marrewijk, J, Vargas, C, Vavagiakis, E, Wagoner, K, Wang, Y, Wenzl, L, Wollack, E, Xu, Z, Zago, F, Zheng, K, Madhavacheril M. S., Qu F. J., Sherwin B. D., MacCrann N., Li Y., Abril-Cabezas I., Ade P. A. R., Aiola S., Alford T., Amiri M., Amodeo S., An R., Atkins Z., Austermann J. E., Battaglia N., Battistelli E. S., Beall J. A., Bean R., Beringue B., Bhandarkar T., Biermann E., Bolliet B., Bond J. R., Cai H., Calabrese E., Calafut V., Capalbo V., Carrero F., Challinor A., Chesmore G. E., Cho H. -M., Choi S. K., Clark S. E., Rosado R. C., Cothard N. F., Coughlin K., Coulton W., Crowley K. T., Dalal R., Darwish O., Devlin M. J., Dicker S., Doze P., Duell C. J., Duff S. M., Duivenvoorden A. J., Dunkley J., Dunner R., Fanfani V., Fankhanel M., Farren G., Ferraro S., Freundt R., Fuzia B., Gallardo P. A., Garrido X., Givans J., Gluscevic V., Golec J. E., Guan Y., Hall K. R., Halpern M., Han D., Harrison I., Hasselfield M., Healy E., Henderson S., Hensley B., Hervias-Caimapo C., Hill J. C., Hilton G. C., Hilton M., Hincks A. D., Hlozek R., Ho S. P., Huber Z. B., Hubmayr J., Huffenberger K. M., Hughes J. P., Irwin K., Isopi G., Jense H. T., Keller B., Kim J., Knowles K., Koopman B. J., Kosowsky A., Kramer D., Kusiak A., La Posta A., Lague A., Lakey V., Lee E., Li Z., Limon M., Lokken M., Louis T., Lungu M., MacInnis A., Maldonado D., Maldonado F., Mallaby-Kay M., Marques G. A., McMahon J., Mehta Y., Menanteau F., Moodley K., Morris T. W., Mroczkowski T., Naess S., Namikawa T., Nati F., Newburgh L., Nicola A., Niemack M. D., Nolta M. R., Orlowski-Scherer J., Page L. A., Pandey S., Partridge B., Prince H., Puddu R., Radiconi F., Robertson N., Rojas F., Sakuma T., Salatino M., Schaan E., Schmitt B. L., Sehgal N., Shaikh S., Sierra C., Sievers J., Sifon C., Simon S., Sonka R., Spergel D. N., Staggs S. T., Storer E., Switzer E. R., Tampier N., Thornton R., Trac H., Treu J., Tucker C., Ullom J., Vale L. R., Van Engelen A., Van Lanen J., van Marrewijk J., Vargas C., Vavagiakis E. M., Wagoner K., Wang Y., Wenzl L., Wollack E. J., Xu Z., Zago F., and Zheng K.

Published
2024

12. The Atacama Cosmology Telescope: A Measurement of the DR6 CMB Lensing Power Spectrum and Its Implications for Structure Growth

Author

Qu, F, Sherwin, B, Madhavacheril, M, Han, D, Crowley, K, Abril-Cabezas, I, Ade, P, Aiola, S, Alford, T, Amiri, M, Amodeo, S, An, R, Atkins, Z, Austermann, J, Battaglia, N, Battistelli, E, Beall, J, Bean, R, Beringue, B, Bhandarkar, T, Biermann, E, Bolliet, B, Bond, J, Cai, H, Calabrese, E, Calafut, V, Capalbo, V, Carrero, F, Carron, J, Challinor, A, Chesmore, G, Cho, H, Choi, S, Clark, S, Rosado, R, Cothard, N, Coughlin, K, Coulton, W, Dalal, R, Darwish, O, Devlin, M, Dicker, S, Doze, P, Duell, C, Duff, S, Duivenvoorden, A, Dunkley, J, Dunner, R, Fanfani, V, Fankhanel, M, Farren, G, Ferraro, S, Freundt, R, Fuzia, B, Gallardo, P, Garrido, X, Gluscevic, V, Golec, J, Guan, Y, Halpern, M, Harrison, I, Hasselfield, M, Healy, E, Henderson, S, Hensley, B, Hervias-Caimapo, C, Hill, J, Hilton, G, Hilton, M, Hincks, A, Hlozek, R, Ho, S, Huber, Z, Hubmayr, J, Huffenberger, K, Hughes, J, Irwin, K, Isopi, G, Jense, H, Keller, B, Kim, J, Knowles, K, Koopman, B, Kosowsky, A, Kramer, D, Kusiak, A, La Posta, A, Lague, A, Lakey, V, Lee, E, Li, Z, Li, Y, Limon, M, Lokken, M, Louis, T, Lungu, M, Maccrann, N, Macinnis, A, Maldonado, D, Maldonado, F, Mallaby-Kay, M, Marques, G, Mcmahon, J, Mehta, Y, Menanteau, F, Moodley, K, Morris, T, Mroczkowski, T, Naess, S, Namikawa, T, Nati, F, Newburgh, L, Nicola, A, Niemack, M, Nolta, M, Orlowski-Scherer, J, Page, L, Pandey, S, Partridge, B, Prince, H, Puddu, R, Radiconi, F, Robertson, N, Rojas, F, Sakuma, T, Salatino, M, Schaan, E, Schmitt, B, Sehgal, N, Shaikh, S, Sierra, C, Sievers, J, Sifon, C, Simon, S, Sonka, R, Spergel, D, Staggs, S, Storer, E, Switzer, E, Tampier, N, Thornton, R, Trac, H, Treu, J, Tucker, C, Ullom, J, Vale, L, Van Engelen, A, Van Lanen, J, van Marrewijk, J, Vargas, C, Vavagiakis, E, Wagoner, K, Wang, Y, Wenzl, L, Wollack, E, Xu, Z, Zago, F, Zheng, K, Qu F. J., Sherwin B. D., Madhavacheril M. S., Han D., Crowley K. T., Abril-Cabezas I., Ade P. A. R., Aiola S., Alford T., Amiri M., Amodeo S., An R., Atkins Z., Austermann J. E., Battaglia N., Battistelli E. S., Beall J. A., Bean R., Beringue B., Bhandarkar T., Biermann E., Bolliet B., Bond J. R., Cai H., Calabrese E., Calafut V., Capalbo V., Carrero F., Carron J., Challinor A., Chesmore G. E., Cho H. -M., Choi S. K., Clark S. E., Rosado R. C., Cothard N. F., Coughlin K., Coulton W., Dalal R., Darwish O., Devlin M. J., Dicker S., Doze P., Duell C. J., Duff S. M., Duivenvoorden A. J., Dunkley J., Dunner R., Fanfani V., Fankhanel M., Farren G., Ferraro S., Freundt R., Fuzia B., Gallardo P. A., Garrido X., Gluscevic V., Golec J. E., Guan Y., Halpern M., Harrison I., Hasselfield M., Healy E., Henderson S., Hensley B., Hervias-Caimapo C., Hill J. C., Hilton G. C., Hilton M., Hincks A. D., Hlozek R., Ho S. P., Huber Z. B., Hubmayr J., Huffenberger K. M., Hughes J. P., Irwin K., Isopi G., Jense H. T., Keller B., Kim J., Knowles K., Koopman B. J., Kosowsky A., Kramer D., Kusiak A., La Posta A., Lague A., Lakey V., Lee E., Li Z., Li Y., Limon M., Lokken M., Louis T., Lungu M., MacCrann N., MacInnis A., Maldonado D., Maldonado F., Mallaby-Kay M., Marques G. A., McMahon J., Mehta Y., Menanteau F., Moodley K., Morris T. W., Mroczkowski T., Naess S., Namikawa T., Nati F., Newburgh L., Nicola A., Niemack M. D., Nolta M. R., Orlowski-Scherer J., Page L. A., Pandey S., Partridge B., Prince H., Puddu R., Radiconi F., Robertson N., Rojas F., Sakuma T., Salatino M., Schaan E., Schmitt B. L., Sehgal N., Shaikh S., Sierra C., Sievers J., Sifon C., Simon S., Sonka R., Spergel D. N., Staggs S. T., Storer E., Switzer E. R., Tampier N., Thornton R., Trac H., Treu J., Tucker C., Ullom J., Vale L. R., Van Engelen A., Van Lanen J., van Marrewijk J., Vargas C., Vavagiakis E. M., Wagoner K., Wang Y., Wenzl L., Wollack E. J., Xu Z., Zago F., Zheng K., Qu, F, Sherwin, B, Madhavacheril, M, Han, D, Crowley, K, Abril-Cabezas, I, Ade, P, Aiola, S, Alford, T, Amiri, M, Amodeo, S, An, R, Atkins, Z, Austermann, J, Battaglia, N, Battistelli, E, Beall, J, Bean, R, Beringue, B, Bhandarkar, T, Biermann, E, Bolliet, B, Bond, J, Cai, H, Calabrese, E, Calafut, V, Capalbo, V, Carrero, F, Carron, J, Challinor, A, Chesmore, G, Cho, H, Choi, S, Clark, S, Rosado, R, Cothard, N, Coughlin, K, Coulton, W, Dalal, R, Darwish, O, Devlin, M, Dicker, S, Doze, P, Duell, C, Duff, S, Duivenvoorden, A, Dunkley, J, Dunner, R, Fanfani, V, Fankhanel, M, Farren, G, Ferraro, S, Freundt, R, Fuzia, B, Gallardo, P, Garrido, X, Gluscevic, V, Golec, J, Guan, Y, Halpern, M, Harrison, I, Hasselfield, M, Healy, E, Henderson, S, Hensley, B, Hervias-Caimapo, C, Hill, J, Hilton, G, Hilton, M, Hincks, A, Hlozek, R, Ho, S, Huber, Z, Hubmayr, J, Huffenberger, K, Hughes, J, Irwin, K, Isopi, G, Jense, H, Keller, B, Kim, J, Knowles, K, Koopman, B, Kosowsky, A, Kramer, D, Kusiak, A, La Posta, A, Lague, A, Lakey, V, Lee, E, Li, Z, Li, Y, Limon, M, Lokken, M, Louis, T, Lungu, M, Maccrann, N, Macinnis, A, Maldonado, D, Maldonado, F, Mallaby-Kay, M, Marques, G, Mcmahon, J, Mehta, Y, Menanteau, F, Moodley, K, Morris, T, Mroczkowski, T, Naess, S, Namikawa, T, Nati, F, Newburgh, L, Nicola, A, Niemack, M, Nolta, M, Orlowski-Scherer, J, Page, L, Pandey, S, Partridge, B, Prince, H, Puddu, R, Radiconi, F, Robertson, N, Rojas, F, Sakuma, T, Salatino, M, Schaan, E, Schmitt, B, Sehgal, N, Shaikh, S, Sierra, C, Sievers, J, Sifon, C, Simon, S, Sonka, R, Spergel, D, Staggs, S, Storer, E, Switzer, E, Tampier, N, Thornton, R, Trac, H, Treu, J, Tucker, C, Ullom, J, Vale, L, Van Engelen, A, Van Lanen, J, van Marrewijk, J, Vargas, C, Vavagiakis, E, Wagoner, K, Wang, Y, Wenzl, L, Wollack, E, Xu, Z, Zago, F, Zheng, K, Qu F. J., Sherwin B. D., Madhavacheril M. S., Han D., Crowley K. T., Abril-Cabezas I., Ade P. A. R., Aiola S., Alford T., Amiri M., Amodeo S., An R., Atkins Z., Austermann J. E., Battaglia N., Battistelli E. S., Beall J. A., Bean R., Beringue B., Bhandarkar T., Biermann E., Bolliet B., Bond J. R., Cai H., Calabrese E., Calafut V., Capalbo V., Carrero F., Carron J., Challinor A., Chesmore G. E., Cho H. -M., Choi S. K., Clark S. E., Rosado R. C., Cothard N. F., Coughlin K., Coulton W., Dalal R., Darwish O., Devlin M. J., Dicker S., Doze P., Duell C. J., Duff S. M., Duivenvoorden A. J., Dunkley J., Dunner R., Fanfani V., Fankhanel M., Farren G., Ferraro S., Freundt R., Fuzia B., Gallardo P. A., Garrido X., Gluscevic V., Golec J. E., Guan Y., Halpern M., Harrison I., Hasselfield M., Healy E., Henderson S., Hensley B., Hervias-Caimapo C., Hill J. C., Hilton G. C., Hilton M., Hincks A. D., Hlozek R., Ho S. P., Huber Z. B., Hubmayr J., Huffenberger K. M., Hughes J. P., Irwin K., Isopi G., Jense H. T., Keller B., Kim J., Knowles K., Koopman B. J., Kosowsky A., Kramer D., Kusiak A., La Posta A., Lague A., Lakey V., Lee E., Li Z., Li Y., Limon M., Lokken M., Louis T., Lungu M., MacCrann N., MacInnis A., Maldonado D., Maldonado F., Mallaby-Kay M., Marques G. A., McMahon J., Mehta Y., Menanteau F., Moodley K., Morris T. W., Mroczkowski T., Naess S., Namikawa T., Nati F., Newburgh L., Nicola A., Niemack M. D., Nolta M. R., Orlowski-Scherer J., Page L. A., Pandey S., Partridge B., Prince H., Puddu R., Radiconi F., Robertson N., Rojas F., Sakuma T., Salatino M., Schaan E., Schmitt B. L., Sehgal N., Shaikh S., Sierra C., Sievers J., Sifon C., Simon S., Sonka R., Spergel D. N., Staggs S. T., Storer E., Switzer E. R., Tampier N., Thornton R., Trac H., Treu J., Tucker C., Ullom J., Vale L. R., Van Engelen A., Van Lanen J., van Marrewijk J., Vargas C., Vavagiakis E. M., Wagoner K., Wang Y., Wenzl L., Wollack E. J., Xu Z., Zago F., and Zheng K.

Published
2024

13. Atacama Cosmology Telescope: High-resolution component-separated maps across one third of the sky

Author

Coulton, W, Madhavacheril, M, Duivenvoorden, A, Hill, J, Abril-Cabezas, I, Ade, P, Aiola, S, Alford, T, Amiri, M, Amodeo, S, An, R, Atkins, Z, Austermann, J, Battaglia, N, Battistelli, E, Beall, J, Bean, R, Beringue, B, Bhandarkar, T, Biermann, E, Bolliet, B, Bond, J, Cai, H, Calabrese, E, Calafut, V, Capalbo, V, Carrero, F, Chesmore, G, Cho, H, Choi, S, Clark, S, Rosado, R, Cothard, N, Coughlin, K, Crowley, K, Devlin, M, Dicker, S, Doze, P, Duell, C, Duff, S, Dunkley, J, Dünner, R, Fanfani, V, Fankhanel, M, Farren, G, Ferraro, S, Freundt, R, Fuzia, B, Gallardo, P, Garrido, X, Givans, J, Gluscevic, V, Golec, J, Guan, Y, Halpern, M, Han, D, Hasselfield, M, Healy, E, Henderson, S, Hensley, B, Hervías-Caimapo, C, Hilton, G, Hilton, M, Hincks, A, Hložek, R, Ho, S, Huber, Z, Hubmayr, J, Huffenberger, K, Hughes, J, Irwin, K, Isopi, G, Jense, H, Keller, B, Kim, J, Knowles, K, Koopman, B, Kosowsky, A, Kramer, D, Kusiak, A, La Posta, A, Lakey, V, Lee, E, Li, Z, Li, Y, Limon, M, Lokken, M, Louis, T, Lungu, M, Maccrann, N, Macinnis, A, Maldonado, D, Maldonado, F, Mallaby-Kay, M, Marques, G, Van Marrewijk, J, Mccarthy, F, Mcmahon, J, Mehta, Y, Menanteau, F, Coulton W., Madhavacheril M. S., Duivenvoorden A. J., Hill J. C., Abril-Cabezas I., Ade P. A. R., Aiola S., Alford T., Amiri M., Amodeo S., An R., Atkins Z., Austermann J. E., Battaglia N., Battistelli E. S., Beall J. A., Bean R., Beringue B., Bhandarkar T., Biermann E., Bolliet B., Bond J. R., Cai H., Calabrese E., Calafut V., Capalbo V., Carrero F., Chesmore G. E., Cho H. M., Choi S. K., Clark S. E., Rosado R. C., Cothard N. F., Coughlin K., Crowley K. T., Devlin M. J., Dicker S., Doze P., Duell C. J., Duff S. M., Dunkley J., Dünner R., Fanfani V., Fankhanel M., Farren G., Ferraro S., Freundt R., Fuzia B., Gallardo P. A., Garrido X., Givans J., Gluscevic V., Golec J. E., Guan Y., Halpern M., Han D., Hasselfield M., Healy E., Henderson S., Hensley B., Hervías-Caimapo C., Hilton G. C., Hilton M., Hincks A. D., HloŽek R., Ho S. P. P., Huber Z. B., Hubmayr J., Huffenberger K. M., Hughes J. P., Irwin K., Isopi G., Jense H. T., Keller B., Kim J., Knowles K., Koopman B. J., Kosowsky A., Kramer D., Kusiak A., La Posta A., Lakey V., Lee E., Li Z., Li Y., Limon M., Lokken M., Louis T., Lungu M., Maccrann N., Macinnis A., Maldonado D., Maldonado F., Mallaby-Kay M., Marques G. A., Van Marrewijk J., McCarthy F., McMahon J., Mehta Y., Menanteau F., Coulton, W, Madhavacheril, M, Duivenvoorden, A, Hill, J, Abril-Cabezas, I, Ade, P, Aiola, S, Alford, T, Amiri, M, Amodeo, S, An, R, Atkins, Z, Austermann, J, Battaglia, N, Battistelli, E, Beall, J, Bean, R, Beringue, B, Bhandarkar, T, Biermann, E, Bolliet, B, Bond, J, Cai, H, Calabrese, E, Calafut, V, Capalbo, V, Carrero, F, Chesmore, G, Cho, H, Choi, S, Clark, S, Rosado, R, Cothard, N, Coughlin, K, Crowley, K, Devlin, M, Dicker, S, Doze, P, Duell, C, Duff, S, Dunkley, J, Dünner, R, Fanfani, V, Fankhanel, M, Farren, G, Ferraro, S, Freundt, R, Fuzia, B, Gallardo, P, Garrido, X, Givans, J, Gluscevic, V, Golec, J, Guan, Y, Halpern, M, Han, D, Hasselfield, M, Healy, E, Henderson, S, Hensley, B, Hervías-Caimapo, C, Hilton, G, Hilton, M, Hincks, A, Hložek, R, Ho, S, Huber, Z, Hubmayr, J, Huffenberger, K, Hughes, J, Irwin, K, Isopi, G, Jense, H, Keller, B, Kim, J, Knowles, K, Koopman, B, Kosowsky, A, Kramer, D, Kusiak, A, La Posta, A, Lakey, V, Lee, E, Li, Z, Li, Y, Limon, M, Lokken, M, Louis, T, Lungu, M, Maccrann, N, Macinnis, A, Maldonado, D, Maldonado, F, Mallaby-Kay, M, Marques, G, Van Marrewijk, J, Mccarthy, F, Mcmahon, J, Mehta, Y, Menanteau, F, Coulton W., Madhavacheril M. S., Duivenvoorden A. J., Hill J. C., Abril-Cabezas I., Ade P. A. R., Aiola S., Alford T., Amiri M., Amodeo S., An R., Atkins Z., Austermann J. E., Battaglia N., Battistelli E. S., Beall J. A., Bean R., Beringue B., Bhandarkar T., Biermann E., Bolliet B., Bond J. R., Cai H., Calabrese E., Calafut V., Capalbo V., Carrero F., Chesmore G. E., Cho H. M., Choi S. K., Clark S. E., Rosado R. C., Cothard N. F., Coughlin K., Crowley K. T., Devlin M. J., Dicker S., Doze P., Duell C. J., Duff S. M., Dunkley J., Dünner R., Fanfani V., Fankhanel M., Farren G., Ferraro S., Freundt R., Fuzia B., Gallardo P. A., Garrido X., Givans J., Gluscevic V., Golec J. E., Guan Y., Halpern M., Han D., Hasselfield M., Healy E., Henderson S., Hensley B., Hervías-Caimapo C., Hilton G. C., Hilton M., Hincks A. D., HloŽek R., Ho S. P. P., Huber Z. B., Hubmayr J., Huffenberger K. M., Hughes J. P., Irwin K., Isopi G., Jense H. T., Keller B., Kim J., Knowles K., Koopman B. J., Kosowsky A., Kramer D., Kusiak A., La Posta A., Lakey V., Lee E., Li Z., Li Y., Limon M., Lokken M., Louis T., Lungu M., Maccrann N., Macinnis A., Maldonado D., Maldonado F., Mallaby-Kay M., Marques G. A., Van Marrewijk J., McCarthy F., McMahon J., Mehta Y., and Menanteau F.

Abstract

Observations of the millimeter sky contain valuable information on a number of signals, including the blackbody cosmic microwave background (CMB), Galactic emissions, and the Compton-y distortion due to the thermal Sunyaev-Zel'dovich (tSZ) effect. Extracting new insight into cosmological and astrophysical questions often requires combining multiwavelength observations to spectrally isolate one component. In this work, we present a new arc-minute-resolution Compton-y map, which traces out the line-of-sight-integrated electron pressure, as well as maps of the CMB in intensity and E-mode polarization, across a third of the sky (around 13,000 deg2). We produce these through a joint analysis of data from the Atacama Cosmology Telescope (ACT) data release 4 and 6 at frequencies of roughly 93, 148, and 225 GHz, together with data from the Planck satellite at frequencies between 30 and 545 GHz. We present detailed verification of an internal linear combination pipeline implemented in a needlet frame that allows us to efficiently suppress Galactic contamination and account for spatial variations in the ACT instrument noise. These maps provide a significant advance, in noise levels and resolution, over the existing Planck component-separated maps and will enable a host of science goals including studies of cluster and galaxy astrophysics, inferences of the cosmic velocity field, primordial non-Gaussianity searches, and gravitational lensing reconstruction of the CMB.

Published
2024

14. The Simons Observatory: Science goals and forecasts

Author

Ade, P, Aguirre, J, Ahmed, Z, Aiola, S, Ali, A, Alonso, D, Alvarez, MA, Arnold, K, Ashton, P, Austermann, J, Awan, H, Baccigalupi, C, Baildon, T, Barron, D, Battaglia, N, Battye, R, Baxter, E, Bazarko, A, Beall, JA, Bean, R, Beck, D, Beckman, S, Beringue, B, Bianchini, F, Boada, S, Boettger, D, Bond, JR, Borrill, J, Brown, ML, Bruno, SM, Bryan, S, Calabrese, E, Calafut, V, Calisse, P, Carron, J, Challinor, A, Chesmore, G, Chinone, Y, Chluba, J, Cho, HMS, Choi, S, Coppi, G, Cothard, NF, Coughlin, K, Crichton, D, Crowley, KD, Crowley, KT, Cukierman, A, D'Ewart, JM, Dünner, R, De Haan, T, Devlin, M, Dicker, S, Didier, J, Dobbs, M, Dober, B, Duell, CJ, Duff, S, Duivenvoorden, A, Dunkley, J, Dusatko, J, Errard, J, Fabbian, G, Feeney, S, Ferraro, S, Fluxà, P, Freese, K, Frisch, JC, Frolov, A, Fuller, G, Fuzia, B, Galitzki, N, Gallardo, PA, Ghersi, JTG, Gao, J, Gawiser, E, Gerbino, M, Gluscevic, V, Goeckner-Wald, N, Golec, J, Gordon, S, Gralla, M, Green, D, Grigorian, A, Groh, J, Groppi, C, Guan, Y, Gudmundsson, JE, Han, D, Hargrave, P, Hasegawa, M, Hasselfield, M, Hattori, M, Haynes, V, Hazumi, M, He, Y, Healy, E, Henderson, SW, Hervias-Caimapo, C, and Hill, CA

Subjects
CMBR experiments, CMBR polarisation, cosmological parameters from CMBR, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Nuclear & Particles Physics, Atomic, Molecular, Nuclear, Particle and Plasma Physics
Abstract

The Simons Observatory (SO) is a new cosmic microwave background experiment being built on Cerro Toco in Chile, due to begin observations in the early 2020s. We describe the scientific goals of the experiment, motivate the design, and forecast its performance. SO will measure the temperature and polarization anisotropy of the cosmic microwave background in six frequency bands centered at: 27, 39, 93, 145, 225 and 280 GHz. The initial configuration of SO will have three small-aperture 0.5-m telescopes and one large-aperture 6-m telescope, with a total of 60,000 cryogenic bolometers. Our key science goals are to characterize the primordial perturbations, measure the number of relativistic species and the mass of neutrinos, test for deviations from a cosmological constant, improve our understanding of galaxy evolution, and constrain the duration of reionization. The small aperture telescopes will target the largest angular scales observable from Chile, mapping 10% of the sky to a white noise level of 2 μK-arcmin in combined 93 and 145 GHz bands, to measure the primordial tensor-to-scalar ratio, r, at a target level of σ(r)=0.003. The large aperture telescope will map 40% of the sky at arcminute angular resolution to an expected white noise level of 6 μK-arcmin in combined 93 and 145 GHz bands, overlapping with the majority of the Large Synoptic Survey Telescope sky region and partially with the Dark Energy Spectroscopic Instrument. With up to an order of magnitude lower polarization noise than maps from the Planck satellite, the high-resolution sky maps will constrain cosmological parameters derived from the damping tail, gravitational lensing of the microwave background, the primordial bispectrum, and the thermal and kinematic Sunyaev-Zel'dovich effects, and will aid in delensing the large-angle polarization signal to measure the tensor-to-scalar ratio. The survey will also provide a legacy catalog of 16,000 galaxy clusters and more than 20,000 extragalactic sources.

Published
2019

16. The Whole is Greater than the Sum of the Parts: Optimizing the Joint Science Return from LSST, Euclid and WFIRST

Author

Jain, B., Spergel, D., Bean, R., Connolly, A., Dell'antonio, I., Frieman, J., Gawiser, E., Gehrels, N., Gladney, L., Heitmann, K., Helou, G., Hirata, C., Ho, S., Ivezić, Ž., Jarvis, M., Kahn, S., Kalirai, J., Kim, A., Lupton, R., Mandelbaum, R., Marshall, P., Newman, J. A., Perlmutter, S., Postman, M., Rhodes, J., Strauss, M. A., Tyson, J. A., Walkowicz, L., and Wood-Vasey, W. M.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The focus of this report is on the opportunities enabled by the combination of LSST, Euclid and WFIRST, the optical surveys that will be an essential part of the next decade's astronomy. The sum of these surveys has the potential to be significantly greater than the contributions of the individual parts. As is detailed in this report, the combination of these surveys should give us multi-wavelength high-resolution images of galaxies and broadband data covering much of the stellar energy spectrum. These stellar and galactic data have the potential of yielding new insights into topics ranging from the formation history of the Milky Way to the mass of the neutrino. However, enabling the astronomy community to fully exploit this multi-instrument data set is a challenging technical task: for much of the science, we will need to combine the photometry across multiple wavelengths with varying spectral and spatial resolution. We identify some of the key science enabled by the combined surveys and the key technical challenges in achieving the synergies., Comment: Whitepaper developed at June 2014 U. Penn Workshop; 28 pages, 3 figures

Published
2015

17. Operational experience with Adaptive Gain Integrating Pixel Detectors at European XFEL

Author

Sztuk-Dambietz, J., Rovensky, V., Klujev, A., Laurus, T., Trunk, U., Ahmed, K., Meyer, O., Möller, J., Parenti, A., Raab, N., Shayduk, R., Sikorski, M., Ansaldi, G., Bösenberg, U., Luis, L. M., Muenich, A., Preston, T. R., Schmidt, P., Stern, S., Bean, R., Madsen, A., Gelisio, L., Hauf, S., Gessler, P., Wrona, K., Graafsma, Heinz, Turcato, M., Sztuk-Dambietz, J., Rovensky, V., Klujev, A., Laurus, T., Trunk, U., Ahmed, K., Meyer, O., Möller, J., Parenti, A., Raab, N., Shayduk, R., Sikorski, M., Ansaldi, G., Bösenberg, U., Luis, L. M., Muenich, A., Preston, T. R., Schmidt, P., Stern, S., Bean, R., Madsen, A., Gelisio, L., Hauf, S., Gessler, P., Wrona, K., Graafsma, Heinz, and Turcato, M.

Abstract

The European X-ray Free Electron Laser (European XFEL) is a cutting-edge user facility that generates per second up to 27,000 ultra-short, spatially coherent X-ray pulses within an energy range of 0.26 to more than 20 keV. Specialized instrumentation, including various 2D X-ray detectors capable of handling the unique time structure of the beam, is required. The one-megapixel AGIPD (AGIPD1M) detectors, developed for the European XFEL by the AGIPD Consortium, are the primary detectors used for user experiments at the SPB/SFX and MID instruments. The first AGIPD1M detector was installed at SPB/SFX when the facility began operation in 2017, and the second one was installed at MID in November 2018. The AGIPD detector systems require a dedicated infrastructure, well-defined safety systems, and high-level control procedures to ensure stable and safe operation. As of now, the AGIPD1M detectors installed at the SPB/SFX and MID experimental end stations are fully integrated into the European XFEL environment, including mechanical integration, vacuum, power, control, data acquisition, and data processing systems. Specific high-level procedures allow facilitated detector control, and dedicated interlock systems based on Programmable Logic Controllers ensure detector safety in case of power, vacuum, or cooling failure. The first 6 years of operation have clearly demonstrated that the AGIPD1M detectors provide high-quality scientific results. The collected data, along with additional dedicated studies, have also enabled the identification and quantification of issues related to detector performance, ensuring stable operation. Characterization and calibration of detectors are among the most critical and challenging aspects of operation due to their complex nature. A methodology has been developed to enable detector characterization and data correction, both in near real-time (online) and offline mode. The calibration process optimizes detector performance and ensures the highest

Published
2024
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18. X-ray imaging and multiferroic coupling of cycloidal magnetic domains in ferroelectric monodomain BiFeO3

Author

Johnson, R. D., Barone, P., Bombardi, A., Bean, R. J., Picozzi, S., Radaelli, P. G., Oh, Y. S., Cheong, S-W., and Chapon, L. C.

Subjects
Condensed Matter - Strongly Correlated Electrons
Abstract

Magnetic domains at the surface of a ferroelectric monodomain BiFeO3 single crystal have been imaged by hard X-ray magnetic scattering. Magnetic domains up to several hundred microns in size have been observed, corresponding to cycloidal modulations of the magnetization along the wave-vector k=2\pi(\delta,\delta,0) and symmetry equivalent directions. The rotation direction of the magnetization in all magnetic domains, determined by diffraction of circularly polarized light, was found to be unique and in agreement with predictions of a combined approach based on a spin-model complemented by relativistic density-functional simulations. Imaging of the surface shows that the largest adjacent domains display a 120 degree vortex structure., Comment: Published in Physical Review Letters

Published
2013
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29. Wide-Field InfraRed Survey Telescope (WFIRST) Final Report

Author

Green, J., Schechter, P., Baltay, C., Bean, R., Bennett, D., Brown, R., Conselice, C., Donahue, M., Fan, X., Gaudi, B. S., Hirata, C., Kalirai, J., Lauer, T., Nichol, B., Padmanabhan, N., Perlmutter, S., Rauscher, B., Rhodes, J., Roellig, T., Stern, D., Sumi, T., Tanner, A., Wang, Y., Weinberg, D., Wright, E., Gehrels, N., Sambruna, R., Traub, W., Anderson, J., Cook, K., Garnavich, P., Hillenbrand, L., Ivezic, Z., Kerins, E., Lunine, J., McDonald, P., Penny, M., Phillips, M., Rieke, G., Riess, A., van der Marel, R., Barry, R. K., Cheng, E., Content, D., Cutri, R., Goullioud, R., Grady, K., Helou, G., Jackson, C., Kruk, J., Melton, M., Peddie, C., Rioux, N., and Seiffert, M.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

In December 2010, NASA created a Science Definition Team (SDT) for WFIRST, the Wide Field Infra-Red Survey Telescope, recommended by the Astro 2010 Decadal Survey as the highest priority for a large space mission. The SDT was chartered to work with the WFIRST Project Office at GSFC and the Program Office at JPL to produce a Design Reference Mission (DRM) for WFIRST. Part of the original charge was to produce an interim design reference mission by mid-2011. That document was delivered to NASA and widely circulated within the astronomical community. In late 2011 the Astrophysics Division augmented its original charge, asking for two design reference missions. The first of these, DRM1, was to be a finalized version of the interim DRM, reducing overall mission costs where possible. The second of these, DRM2, was to identify and eliminate capabilities that overlapped with those of NASA's James Webb Space Telescope (henceforth JWST), ESA's Euclid mission, and the NSF's ground-based Large Synoptic Survey Telescope (henceforth LSST), and again to reduce overall mission cost, while staying faithful to NWNH. This report presents both DRM1 and DRM2., Comment: 102 pages, 57 figures, 17 tables

Published
2012

30. Erratum: Atacama Cosmology Telescope: Modeling the gas thermodynamics in BOSS CMASS galaxies from kinematic and thermal Sunyaev-Zel'dovich measurements (Phys. Rev. D (2021) 103 (063514) DOI: 10.1103/PhysRevD.103.063514)

Author

Amodeo S., Amodeo, S, Battaglia, N, Schaan, E, Ferraro, S, Moser, E, Aiola, S, Austermann, J, Beall, J, Bean, R, Becker, D, Bond, R, Calabrese, E, Calafut, V, Choi, S, Denison, E, Devlin, M, Duff, S, Duivenvoorden, A, Dunkley, J, Dünner, R, Gallardo, P, Hall, K, Han, D, Hill, J, Hilton, G, Hilton, M, Hložek, R, Hubmayr, J, Huffenberger, K, Hughes, J, Koopman, B, Macinnis, A, Mcmahon, J, Madhavacheril, M, Moodley, K, Mroczkowski, T, Naess, S, Nati, F, Newburgh, L, Niemack, M, Page, L, Partridge, B, Schillaci, A, Sehgal, N, Sifón, C, Spergel, D, Staggs, S, Storer, E, Ullom, J, Vale, L, Van Engelen, A, Van Lanen, J, Vavagiakis, E, Wollack, E, Xu, Z, Amodeo S., Battaglia N., Schaan E., Ferraro S., Moser E., Aiola S., Austermann J. E., Beall J. A., Bean R., Becker D. T., Bond R. J., Calabrese E., Calafut V., Choi S. K., Denison E. V., Devlin M., Duff S. M., Duivenvoorden A. J., Dunkley J., Dünner R., Gallardo P. A., Hall K. R., Han D., Hill J. C., Hilton G. C., Hilton M., HloŽek R., Hubmayr J., Huffenberger K. M., Hughes J. P., Koopman B. J., Macinnis A., McMahon J., Madhavacheril M. S., Moodley K., Mroczkowski T., Naess S., Nati F., Newburgh L. B., Niemack M. D., Page L. A., Partridge B., Schillaci A., Sehgal N., Sifón C., Spergel D. N., Staggs S., Storer E. R., Ullom J. N., Vale L. R., Van Engelen A., Van Lanen J., Vavagiakis E. M., Wollack E. J., Xu Z., Amodeo S., Amodeo, S, Battaglia, N, Schaan, E, Ferraro, S, Moser, E, Aiola, S, Austermann, J, Beall, J, Bean, R, Becker, D, Bond, R, Calabrese, E, Calafut, V, Choi, S, Denison, E, Devlin, M, Duff, S, Duivenvoorden, A, Dunkley, J, Dünner, R, Gallardo, P, Hall, K, Han, D, Hill, J, Hilton, G, Hilton, M, Hložek, R, Hubmayr, J, Huffenberger, K, Hughes, J, Koopman, B, Macinnis, A, Mcmahon, J, Madhavacheril, M, Moodley, K, Mroczkowski, T, Naess, S, Nati, F, Newburgh, L, Niemack, M, Page, L, Partridge, B, Schillaci, A, Sehgal, N, Sifón, C, Spergel, D, Staggs, S, Storer, E, Ullom, J, Vale, L, Van Engelen, A, Van Lanen, J, Vavagiakis, E, Wollack, E, Xu, Z, Amodeo S., Battaglia N., Schaan E., Ferraro S., Moser E., Aiola S., Austermann J. E., Beall J. A., Bean R., Becker D. T., Bond R. J., Calabrese E., Calafut V., Choi S. K., Denison E. V., Devlin M., Duff S. M., Duivenvoorden A. J., Dunkley J., Dünner R., Gallardo P. A., Hall K. R., Han D., Hill J. C., Hilton G. C., Hilton M., HloŽek R., Hubmayr J., Huffenberger K. M., Hughes J. P., Koopman B. J., Macinnis A., McMahon J., Madhavacheril M. S., Moodley K., Mroczkowski T., Naess S., Nati F., Newburgh L. B., Niemack M. D., Page L. A., Partridge B., Schillaci A., Sehgal N., Sifón C., Spergel D. N., Staggs S., Storer E. R., Ullom J. N., Vale L. R., Van Engelen A., Van Lanen J., Vavagiakis E. M., Wollack E. J., and Xu Z.

Published
2023

31. Wilkinson Microwave Anisotropy Probe (WMAP) Three Year Results: Implications for Cosmology

Author

Spergel, D. N., Bean, R., Doré, O., Nolta, M. R., Bennett, C. L., Dunkley, J., Hinshaw, G., Jarosik, N., Komatsu, E., Page, L., Peiris, H. V., Verde, L., Halpern, M., Hill, R. S., Kogut, A., Limon, M., Meyer, S. S., Odegard, N., Tucker, G. S., Weiland, J. L., Wollack, E., and Wright, E. L.

Subjects
Astrophysics
Abstract

A simple cosmological model with only six parameters (matter density, Omega_m h^2, baryon density, Omega_b h^2, Hubble Constant, H_0, amplitude of fluctuations, sigma_8, optical depth, tau, and a slope for the scalar perturbation spectrum, n_s) fits not only the three year WMAP temperature and polarization data, but also small scale CMB data, light element abundances, large-scale structure observations, and the supernova luminosity/distance relationship. Using WMAP data only, the best fit values for cosmological parameters for the power-law flat LCDM model are (Omega_m h^2, Omega_b h^2, h, n_s, tau, sigma_8) = 0.1277+0.0080-0.0079, 0.02229+-0.00073, 0.732+0.031-0.032, 0.958+-0.016, 0.089+-0.030, 0.761+0.049-0.048). The three year data dramatically shrink the allowed volume in this six dimensional parameter space. Assuming that the primordial fluctuations are adiabatic with a power law spectrum, the WMAP data_alone_ require dark matter, and favor a spectral index that is significantly less than the Harrison-Zel'dovich-Peebles scale-invariant spectrum (n_s=1, r=0). Models that suppress large-scale power through a running spectral index or a large-scale cut-off in the power spectrum are a better fit to the WMAP and small scale CMB data than the power-law LCDM model; however, the improvement in the fit to the WMAP data is only Delta chi^2 = 3 for 1 extra degree of freedom. The combination of WMAP and other astronomical data yields significant constraints on the geometry of the universe, the equation of state of the dark energy, the gravitational wave energy density, and neutrino properties. Consistent with the predictions of simple inflationary theories, we detect no significant deviations from Gaussianity in the CMB maps., Comment: 91 pgs, 28 figs. Accepted version of the 3-year paper as posted to http://lambda.gsfc.nasa.gov/product/map/dr2/map_bibliography.cfm in January 2007

Published
2006
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32. Three-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Beam Profiles, Data Processing, Radiometer Characterization and Systematic Error Limits

Author

Jarosik, N., Barnes, C., Greason, M. R., Hill, R. S., Nolta, M. R., Odegard, N., Weiland, J. L., Bean, R., Bennett, C. L., Doré, O., Halpern, M., Hinshaw, G., Kogut, A., Komatsu, E., Limon, M., Meyer, S. S., Page, L., Spergel, D. N., Tucker, G. S., Wollack, E., and Wright, E. L.

Subjects
Astrophysics
Abstract

The WMAP satellite has completed 3 years of observations of the cosmic microwave background radiation. The 3-year data products include several sets of full sky maps of the Stokes I, Q and U parameters in 5 frequency bands, spanning 23 to 94 GHz, and supporting items, such as beam window functions and noise covariance matrices. The processing used to produce the current sky maps and supporting products represents a significant advancement over the first year analysis, and is described herein. Improvements to the pointing reconstruction, radiometer gain modeling, window function determination and radiometer spectral noise parametrization are presented. A detailed description of the updated data processing that produces maximum likelihood sky map estimates is presented, along with the methods used to produce reduced resolution maps and corresponding noise covariance matrices. Finally two methods used to evaluate the noise of the full resolution sky maps are presented along with several representative year-to-year null tests, demonstrating that sky maps produced from data from different observational epochs are consistent., Comment: 58 pgs, 16 figs. Accepted version of the 3-year paper as posted on http://lambda.gsfc.nasa.gov/product/map/dr2/map_bibliography.cfm in January 2007

Published
2006
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33. Three-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Temperature Analysis

Author

Hinshaw, G., Nolta, M. R., Bennett, C. L., Bean, R., Doré, O., Greason, M. R., Halpern, M., Hill, R. S., Jarosik, N., Kogut, A., Komatsu, E., Limon, M., Odegard, N., Meyer, S. S., Page, L., Peiris, H. V., Spergel, D. N., Tucker, G. S., Verde, L., Weiland, J. L., Wollack, E., and Wright, E. L.

Subjects
Astrophysics
Abstract

We present new full-sky temperature maps in five frequency bands from 23 to 94 GHz, based on the first three years of the WMAP sky survey. The new maps, which are consistent with the first-year maps and more sensitive, incorporate improvements in data processing made possible by the additional years of data and by a more complete analysis of the polarization signal. These include refinements in the gain calibration and beam response models. We employ two forms of multi-frequency analysis to separate astrophysical foreground signals from the CMB, each of which improves on our first-year analyses. First, we form an improved 'Internal Linear Combination' map, based solely on WMAP data, by adding a bias correction step and by quantifying residual uncertainties in the resulting map. Second, we fit and subtract new spatial templates that trace Galactic emission; in particular, we now use low-frequency WMAP data to trace synchrotron emission. The WMAP point source catalog is updated to include 115 new sources. We derive the angular power spectrum of the temperature anisotropy using a hybrid approach that combines a maximum likelihood estimate at low l (large angular scales) with a quadratic cross-power estimate for l>30. Our best estimate of the CMB power spectrum is derived by averaging cross-power spectra from 153 statistically independent channel pairs. The combined spectrum is cosmic variance limited to l=400, and the signal-to-noise ratio per l-mode exceeds unity up to l=850. The first two acoustic peaks are seen at l=220.8 +- 0.7 and l=530.9 +- 3.8, respectively, while the first two troughs are seen at l=412.4 +- 1.9 and l=675.1 +- 11.1, respectively. The rise to the third peak is unambiguous; when the WMAP data are combined with higher resolution CMB measurements, the existence of a third acoustic peak is well established., Comment: 116 pgs, 24 figs. Accepted version of the 3-year paper as posted to http://lambda.gsfc.nasa.gov/product/map/dr2/map_bibliography.cfm in January 2007

Published
2006
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34. Three Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Polarization Analysis

Author

Page, L., Hinshaw, G., Komatsu, E., Nolta, M. R., Spergel, D. N., Bennett, C. L., Barnes, C., Bean, R., Doré, O., Dunkley, J., Halpern, M., Hill, R. S., Jarosik, N., Kogut, A., Limon, M., Meyer, S. S., Odegard, N., Peiris, H. V., Tucker, G. S., Verde, L., Weiland, J. L., Wollack, E., and Wright, E. L.

Subjects
Astrophysics
Abstract

The Wilkinson Microwave Anisotropy Probe WMAP has mapped the entire sky in five frequency bands between 23 and 94 GHz with polarization sensitive radiometers. We present three-year full-sky maps of the polarization and analyze them for foreground emission and cosmological implications. These observations open up a new window for understanding the universe. WMAP observes significant levels of polarized foreground emission due to both Galactic synchrotron radiation and thermal dust emission. The least contaminated channel is at 61 GHz. Informed by a model of the Galactic foreground emission, we subtract the foreground emission from the maps. In the foreground corrected maps, for l=2-6, we detect l(l+1) C_l^{EE} / (2 pi) = 0.086 +-0.029 microkelvin^2. This is interpreted as the result of rescattering of the CMB by free electrons released during reionization and corresponds to an optical depth of tau = 0.10 +- 0.03. We see no evidence for B-modes, limiting them to l(l+1) C_l^{BB} / (2 pi) = -0.04 +- 0.03 microkelvin^2. We find that the limit from the polarization signals alone is r<2.2 (95% CL) corresponding to a limit on the cosmic density of gravitational waves of Omega_{GW}h^2 < 5 times 10^{-12}. From the full WMAP analysis, we find r<0.55 (95% CL) corresponding to a limit of Omega_{GW}h^2 < 10^{-12} (95% CL)., Comment: 105 pgs, 28 figs. Accepted version of the 3-year paper as posted to http://lambda.gsfc.nasa.gov/product/map/dr2/map_bibliography.cfm in January 2007

Published
2006
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35. Domain structure imaging by Bragg geometry X-ray ptychography

Author

Bean, R. J.

Subjects
500
Abstract

Domain structure in materials is important for their physical properties, technological uses and response to external perturbations. Domains are small regions within a material with a consistent atomic structure that may have different ordering origins or different orientations. Domain structure is present in any material which exhibits super-structure ordering with correlation lengths shorter than the extent of the sample. The domain size is controlled by the strength of the ordering interactions and growth conditions. Domains are present in a huge range of materials from con¬densed matter to biological samples with a structure unique to the individual sample. For domains in crystalline samples with sizes of Angstroms to nanometres X-rays are an ideal probe. Many domain systems exhibit no X-ray amplitude contrast, i.e. all domains attenuate the X-ray beam uniformly, the domain structure is apparent only in the deviation of the phase of the incident X-ray beam. An imaging method is required which is sensitive to these phase differences. Coherent X-ray Diffraction Imaging (CXDI) is a method which exploits the Fourier transform relationship between the sample and its far field diffraction pattern collected at a pixellated detector to iteratively solve the phase problem and reconstruct an amplitude and phase image of the sample. Support based coherent X-ray diffraction methods have been successfully applied to the three dimensional imaging of crystalline structures by collecting the scattering around the sample Bragg peaks in reflection geometry. In general, phase retrieval algorithm constraints require that the sample is isolated within the X-ray beam and as a result these methods have not been successful at imaging extended domain systems. Ptychography is a combined experimental and analysis procedure that can overcome the requirement for the sample to be isolated by collecting a series of diffraction patterns from overlapping regions of the sample. This thesis develops the ptychography algorithms and experimental methods for use in Bragg geometry with the goal of imaging phase domain structures in extended crystalline samples. Bragg coherent diffraction imaging and ptychography methods are reviewed before the adaptations of the experimental method and algorithm for the application of ptychography in Bragg geometry are discussed and detailed. Simulations of ptychography on phase domain structures and a Bragg geometry ptychography X-ray experiment with a specifically designed phase domain test sample confirm that the method is capable of providing accurate quantitative phase information on the domain structure of extended samples. A coherent diffraction experimental setup for ptychography is developed at Diamond beamline I16. Bragg ptychography is applied to the investigation of domain structure in a niobium thin film and anti-phase domain structure in the binary alloy Fe65Al35 and the results of the reconstructions are presented.

Published
2013

36. Measuring $\alpha$ in the Early Universe: CMB Polarization, Reionization and the Fisher Matrix Analysis

Author

Rocha, G., Trotta, R., Martins, C. J. A. P., Melchiorri, A., Avelino, P. P., Bean, R., and Viana, P. T. P.

Subjects
Astrophysics
Abstract

We present a detailed analysis of present and future Cosmic Microwave Background constraints of the value of the fine-structure constant, $\alpha$. We carry out a more detailed analysis of the WMAP first-year data, deriving state-of-the-art constraints on $\alpha$ and discussing various other issues, such as the possible hints for the running of the spectral index. We find, at 95% C.L. that $0.95 < \alpha_{\text{dec}} / \alpha_0 < 1.02$. Setting $dn_S /dlnk=0$, yields $0.94< \alpha_{\text{dec}} / \alpha_0 < 1.01$ as previously reported. We find that a lower value of $\alpha / \alpha_0$ makes a value of $d n_S /dlnk = 0$ more compatible with the data. We also perform a thorough Fisher Matrix Analysis (including both temperature and polarization, as well as $\alpha$ and the optical depth $\tau$), in order to estimate how future CMB experiments will be able to constrain $\alpha$ and other cosmological parameters. We find that Planck data alone can constrain $\tau$ with a accuracy of the order 4% and that this constraint can be as small as 1.7% for an ideal cosmic variance limited experiment. Constraints on $\alpha$ are of the order 0.3% for Planck and can in principle be as small as 0.1% using CMB data alone - tighter constraints will require further (non-CMB) priors., Comment: 29 pages, 11 figures, 15 tables, submitted to MNRAS. Higher resolution figures available at http://www.mrao.cam.ac.uk/~graca/alpha

Published
2003
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37. Measuring $\alpha$ in the Early Universe: CMB Temperature, Large-Scale Structure and Fisher Matrix Analysis

Author

Martins, C. J. A. P., Melchiorri, A., Trotta, R., Bean, R., Rocha, G., Avelino, P. P., and Viana, P. T. P.

Subjects
Astrophysics, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology, High Energy Physics - Theory
Abstract

We extend our recent work on the effects of a time-varying fine-structure constant $\alpha$ in the cosmic microwave background, by providing a thorough analysis of the degeneracies between $\alpha$ and the other cosmological parameters, and discussing ways to break these with both existing and/or forthcoming data. In particular, we present the state-of-the-art CMB constraints on $\alpha$, through a combined analysis of the BOOMERanG, MAXIMA and DASI datasets. We also present a novel discussion of the constraints on $\alpha$ coming from large-scale structure observations, focusing in particular on the power spectrum from the 2dF survey. Our results are consistent with no variation in $\alpha$ from the epoch of recombination to the present day, and restrict any such (relative) variation to be less than about 4%. We show that the forthcoming MAP and (particularly) Planck experiments will be able to break most of the currently existing degeneracies between $\alpha$ and other parameters, and measure $\alpha$ to better than percent accuracy., Comment: 11 pages in RevTex4 format. Low-quality figures to comply with arXiv restrictions (better ones available from the authors). v2: Updated Oklo discussion, plus other cosmetic changes. Version to appear in Phys Rev D

Published
2002
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38. Photographing the wave function of the Universe

Author

Contaldi, C. R., Bean, R., and Magueijo, J.

Subjects
Astrophysics, General Relativity and Quantum Cosmology, High Energy Physics - Theory
Abstract

We show that density fluctuations in standard inflationary scenarios may take the most general non-Gaussian distribution if the wave function of the Universe is not in the ground state. We adopt the Schr\"odinger picture to find a remarkable similarity between the most general inflaton wavefunction and the Edgeworth expansion used in probability theory. Hence we arrive at an explicit relation between the cumulants of the density fluctuations and the amplitudes or occupation numbers of the various energy eigenstates. For incoherent superpositions only even cumulants may be non-zero, but coherent superpositions may generate non-zero odd cumulants as well. Within this framework measurements of cumulants in Galaxy surveys directly map the wavefunction of the Universe., Comment: Replaced with revised version Latex, 10 pages., accepted for publication in Phys. Lett. B

Published
1999
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39. Room temperature crystal structure of the Photoactivated Adenylate Cyclase OaPAC with ATP bound

Author

Chretien, A., primary, Nagel, M.F., additional, Botha, S., additional, de Wijn, R., additional, Brings, L., additional, Doerner, K., additional, Han, H., additional, C.P.Koliyadu, J., additional, Letrun, R., additional, Round, A., additional, Sato, T., additional, Schmidt, C., additional, Secareanu, R., additional, von Stetten, D., additional, Vakili, M., additional, Wrona, A., additional, Bean, R., additional, Mancuso, A., additional, Schulz, J., additional, R.Pearson, A., additional, Kottke, T., additional, Lorenzen, K., additional, and Schubert, R., additional

Published
2023
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40. Cryogenic crystal structure of the Photoactivated Adenylate Cyclase OaPAC with ATP bound

Author

Chretien, A., primary, Nagel, M.F., additional, Botha, S., additional, de Wijn, R., additional, Brings, L., additional, Doerner, K., additional, Han, H., additional, C.P.Koliyadu, J., additional, Letrun, R., additional, Round, A., additional, Sato, T., additional, Schmidt, C., additional, Secareanu, R., additional, von Stetten, D., additional, Vakili, M., additional, Wrona, A., additional, Bean, R., additional, Mancuso, A., additional, Schulz, J., additional, R.Pearson, A., additional, Kottke, T., additional, Lorenzen, K., additional, and Schubert, R., additional

Published
2023
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41. Room temperature crystal structure of the Photoactivated Adenylate Cyclase OaPAC after blue light excitation at 1.8 us delay

Author

Chretien, A., primary, Nagel, M.F., additional, Botha, S., additional, de Wijn, R., additional, Brings, L., additional, Doerner, K., additional, Han, H., additional, C.P.Koliyadu, J., additional, Letrun, R., additional, Sato, T., additional, Round, A., additional, Schmidt, C., additional, Secareanu, R., additional, von Stetten, D., additional, Vakili, M., additional, Wrona, A., additional, Bean, R., additional, Mancuso, A., additional, Schulz, J., additional, R.Pearson, A., additional, Kottke, T., additional, Lorenzen, K., additional, and Schubert, R., additional

Published
2023
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45. Room temperature crystal structure of the Photoactivated Adenylate Cyclase OaPAC after blue light excitation at 2.3 us delay

Author

Chretien, A., primary, Nagel, M.F., additional, Botha, S., additional, de Wijn, R., additional, Brings, L., additional, Doerner, K., additional, Han, H., additional, C.P.Koliyadu, J., additional, Letrun, R., additional, Round, A., additional, Sato, T., additional, Schmidt, C., additional, Secareanu, R., additional, von Stetten, D., additional, Vakili, M., additional, Wrona, A., additional, Bean, R., additional, Mancuso, A., additional, Schulz, J., additional, R.Pearson, A., additional, Kottke, T., additional, Lorenzen, K., additional, and Schubert, R., additional

Published
2023
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46. Cryogenic crystal structure of the Photoactivated Adenylate Cyclase OaPAC

Author

Chretien, A., primary, Nagel, M.F., additional, Botha, S., additional, de Wijn, R., additional, Brings, L., additional, Doerner, K., additional, Han, H., additional, Koliyadu, J., additional, Letrun, R., additional, Round, A., additional, Sato, T., additional, Schmidt, C., additional, Secareanu, R., additional, von Stetten, D., additional, Vakili, M., additional, Wrona, A., additional, Bean, R., additional, Mancuso, A., additional, Schulz, J., additional, Pearson, A., additional, Kottke, T., additional, Lorenzen, K., additional, and Schubert, R., additional

Published
2023
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47. Structural biology of bacterial insecticides using in vivo grown crystals and nanoSFX

Author

Williamson, L., primary, Galchenkova, M., additional, Bean, R., additional, Best, H., additional, Munke, A., additional, Dörner, K., additional, Schubert, R., additional, Bielecki, J., additional, Henkel, A., additional, Yefanov, O., additional, Rizkallah, P. J., additional, Chapman, H. N., additional, Crickmore, N., additional, Berry, C., additional, and Oberthür, D., additional

Published
2023
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50. Oxidized form of SARS-CoV-2 Main Protease determined by XFEL radiation

Author

Schubert, R., primary, Reinke, P., additional, Galchenkova, M., additional, Oberthuer, D., additional, Murillo, G.E.P., additional, Kim, C., additional, Bean, R., additional, Turk, D., additional, Hinrichs, W., additional, Middendorf, P., additional, Round, A., additional, Schmidt, C., additional, Mills, G., additional, Kirkwood, H., additional, Han, H., additional, Koliyadu, J., additional, Bielecki, J., additional, Gelisio, L., additional, Sikorski, M., additional, Kloos, M., additional, Vakilii, M., additional, Yefanov, O.N., additional, Vagovic, P., additional, de-Wijn, R., additional, Letrun, R., additional, Guenther, S., additional, White, T.A., additional, Sato, T., additional, Srinivasan, V., additional, Kim, Y., additional, Chretien, A., additional, Han, S., additional, Brognaro, H., additional, Maracke, J., additional, Knoska, J., additional, Seychell, B.C., additional, Brings, L., additional, Norton-Baker, B., additional, Geng, T., additional, Dore, A.S., additional, Uetrecht, C., additional, Redecke, L., additional, Beck, T., additional, Lorenzen, K., additional, Betzel, C., additional, Mancuso, A.P., additional, Bajt, S., additional, Chapman, H.N., additional, Meents, A., additional, and Lane, T.J., additional

Published
2023
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