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Your search keyword '"Hložek, R."' showing total 11 results
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11 results on '"Hložek, R."'

1. Superclustering with the Atacama Cosmology Telescope and Dark Energy Survey: II. Anisotropic large-scale coherence in hot gas, galaxies, and dark matter

Author

Lokken, M., van Engelen, A., Aguena, M., Allam, S. S., Anbajagane, D., Bacon, D., Baxter, E., Blazek, J., Bocquet, S., Bond, J. R., Brooks, D., Calabrese, E., Rosell, A. Carnero, Carretero, J., Costanzi, M., da Costa, L. N., Coulton, W. R., De Vicente, J., Desai, S., Doel, P., Doux, C., Duivenvoorden, A. J., Dunkley, J., Huang, Z., Everett, S., Ferrero, I., Frieman, J., García-Bellido, J., Gatti, M., Gaztanaga, E., Giannini, G., Gluscevic, V., Gruen, D., Gruendl, R. A., Guan, Y., Gutierrez, G., Hinton, S. R., Hložek, R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Lahav, O., Lee, S., Li, Z., Madhavacheril, M., Marques, G. A., Marshall, J. L., Mena-Fernández, J., Menanteau, F., Miquel, R., Myles, J., Niemack, M. D., Pandey, S., Pereira, M. E. S., Pieres, A., Malagón, A. A. Plazas, Porredon, A., Rodríguez-Monroy, M., Roodman, A., Samuroff, S., Sanchez, E., Cid, D. Sanchez, Santiago, B., Schubnell, M., Sevilla-Noarbe, I., Sifón, C., Smith, M., Staggs, S., Suchyta, E., Swanson, M. E. C., Tarle, G., To, C-H., Weaverdyck, N., Wiseman, P., and Wollack, E. J.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Statistics that capture the directional dependence of the baryon distribution in the cosmic web enable unique tests of cosmology and astrophysical feedback. We use constrained oriented stacking of thermal Sunyaev-Zel'dovich (tSZ) maps to measure the anisotropic distribution of hot gas $2.5-40$ Mpc away from galaxy clusters embedded in massive filaments and superclusters. The cluster selection and orientation (at a scale of $\sim15$ Mpc) use Dark Energy Survey (DES) Year 3 data, while expanded tSZ maps from the Atacama Cosmology Telescope Data Release 6 enable a $\sim3\times$ more significant measurement of the extended gas compared to the technique's proof-of-concept. Decomposing stacks into cosine multipoles of order $m$, we detect a dipole ($m=1$) and quadrupole ($m=2$) at $8-10\sigma$, as well as evidence for $m=4$ signal at up to $6\sigma$, indicating sensitivity to late-time non-Gaussianity. We compare to the Cardinal simulations with spherical gas models pasted onto dark matter halos. The fiducial tSZ data can discriminate between two models that deplete pressure differently in low-mass halos (mimicking astrophysical feedback), preferring higher average pressure in extended structures. However, uncertainty in the amount of cosmic infrared background contamination reduces the constraining power. Additionally, we apply the technique to DES galaxy density and weak lensing to study for the first time their oriented relationships with tSZ. In the tSZ-to-lensing relation, averaged on 7.5 Mpc (transverse) scales, we observe dependence on redshift but not shape or radial distance. Thus, on large scales, the superclustering of gas pressure, galaxies, and total matter is coherent in shape and extent., Comment: 45 pages, 18 figures, submitted to ApJ

Published
2024

2. Evidence for large baryonic feedback at low and intermediate redshifts from kinematic Sunyaev-Zel'dovich observations with ACT and DESI photometric galaxies

Author

Hadzhiyska, B., Ferraro, S., Guachalla, B. Ried, Schaan, E., Aguilar, J., Battaglia, N., Bond, J. R., Brooks, D., Calabrese, E., Choi, S. K., Claybaugh, T., Coulton, W. R., Dawson, K., Devlin, M., Dey, B., Doel, P., Duivenvoorden, A. J., Dunkley, J., Farren, G. S., Font-Ribera, A., Forero-Romero, J. E., Gallardo, P. A., Gaztañaga, E., Gontcho, S. Gontcho, Gralla, M., Guillou, L. Le, Gutierrez, G., Guy, J., Hill, J. C., Hložek, R., Honscheid, K., Juneau, S., Kisner, T., Kremin, A., Landriau, M., Liu, R. H., Louis, T., MacCrann, N., de Macorra, A., Madhavacheril, M., Manera, M., Meisner, A., Miquel, R., Moodley, K., Moustakas, J., Mroczkowski, T., Naess, S., Newman, J., Niemack, M. D., Niz, G., Page, L., Palanque-Delabrouille, N., Partridge, B., Percival, W. J., Prada, F., Qu, F. J., Rossi, G., Sanchez, E., Schlegel, D., Schubnell, M., Sehgal, N., Seo, H., Sifón, C., Spergel, D., Sprayberry, D., Staggs, S., Tarlé, G., Vargas, C., Vavagiakis, E. M., Weaver, B. A., Wollack, E. J., Zhou, R., and Zou, H.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

Recent advances in cosmological observations have provided an unprecedented opportunity to investigate the distribution of baryons relative to the underlying matter. In this work, we robustly show that the gas is much more extended than the dark matter at 40$\sigma$ and the amount of baryonic feedback at $z \lesssim 1$ strongly disfavors low-feedback models such as that of state-of-the-art hydrodynamical simulation IllustrisTNG compared with high-feedback models such as that of the original Illustris simulation. This has important implications for bridging the gap between theory and observations and understanding galaxy formation and evolution. Furthermore, a better grasp of the baryon-dark matter link is critical to future cosmological analyses, which are currently impeded by our limited knowledge of baryonic feedback. Here, we measure the kinematic Sunyaev-Zel'dovich (kSZ) effect from the Atacama Cosmology Telescope (ACT), stacked on the luminous red galaxy (LRG) sample of the Dark Energy Spectroscopic Instrument (DESI) imaging survey. This is the first analysis to use photometric redshifts for reconstructing galaxy velocities. Due to the large number of galaxies comprising the DESI imaging survey, this is the highest signal-to-noise stacked kSZ measurement to date: we detect the signal at 13$\sigma$ and find that the gas is more spread out than the dark matter at $\sim$40$\sigma$. Our work opens up the possibility to recalibrate large hydrodynamical simulations using the kSZ effect. In addition, our findings point towards a way of alleviating inconsistencies between weak lensing surveys and cosmic microwave background (CMB) experiments such as the `low $S_8$' tension, and shed light on long-standing enigmas in astrophysics such as the `missing baryon' problem., Comment: 20 pages, 8 figures, submitting to PRL

Published
2024

3. The LiteBIRD mission to explore cosmic inflation

Author

Ghigna, T., Adler, A., Aizawa, K., Akamatsu, H., Akizawa, R., Allys, E., Anand, A., Aumont, J., Austermann, J., Azzoni, S., Baccigalupi, C., Ballardini, M., Banday, A. J., Barreiro, R. B., Bartolo, N., Basak, S., Basyrov, A., Beckman, S., Bersanelli, M., Bortolami, M., Bouchet, F., Brinckmann, T., Campeti, P., Carinos, E., Carones, A., Casas, F. J., Cheung, K., Chinone, Y., Clermont, L., Columbro, F., Coppolecchia, A., Curtis, D., de Bernardis, P., de Haan, T., de la Hoz, E., De Petris, M., Della Torre, S., Monache, G. Delle, Di Giorgi, E., Dickinson, C., Diego-Palazuelos, P., García, J. J. Díaz, Dobbs, M., Dotani, T., D'Alessandro, G., Eriksen, H. K., Errard, J., Essinger-Hileman, T., Farias, N., Ferreira, E., Franceschet, C., Fuskeland, U., Galloni, G., Galloway, M., Ganga, K., Gerbino, M., Gervasi, M., Génova-Santos, R. T., Giardiello, S., Gimeno-Amo, C., Gjerløw, E., González, R. González, Grandsire, L., Gruppuso, A., Halverson, N. W., Hargrave, P., Harper, S. E., Hazumi, M., Henrot-Versillé, S., Hergt, L. T., Herranz, D., Hivon, E., Hlozek, R. A., Hoang, T. D., Hubmayr, J., Ichiki, K., Ikuma, K., Ishino, H., Jaehnig, G., Jost, B., Kohri, K., Konishi, K., Lamagna, L., Lattanzi, M., Leloup, C., Levrier, F., Lonappan, A. I., Luzzi, G., Macias-Perez, J., Maffei, B., Marchitelli, E., Martínez-González, E., Masi, S., Matarrese, S., Matsumura, T., Micheli, S., Migliaccio, M., Monelli, M., Montier, L., Morgante, G., Mousset, L., Nagano, Y., Nagata, R., Natoli, P., Novelli, A., Noviello, F., Obata, I., Occhiuzzi, A., Odagiri, K., Omae, R., Pagano, L., Paiella, A., Paoletti, D., Pascual-Cisneros, G., Patanchon, G., Pavlidou, V., Piacentini, F., Piat, M., Piccirilli, G., Pinchera, M., Pisano, G., Porcelli, L., Raffuzzi, N., Raum, C., Remazeilles, M., Ritacco, A., Rubino-Martin, J., Ruiz-Granda, M., Sakurai, Y., Savini, G., Scott, D., Sekimoto, Y., Shiraishi, M., Signorelli, G., Stever, S. L., Sullivan, R. M., Suzuki, A., Takaku, R., Takakura, H., Takakura, S., Tartari, Y. Takase. A., Tassis, K., Thompson, K. L., Tomasi, M., Tristram, M., Tucker, C., Vacher, L., van Tent, B., Vielva, P., Watanuki, K., Wehus, I. K., Westbrook, B., Weymann-Despres, G., Winter, B., Wollack, E. J., Zacchei, A., Zannoni, M., Zhou, Y., and Collaboration, the LiteBIRD

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

LiteBIRD, the next-generation cosmic microwave background (CMB) experiment, aims for a launch in Japan's fiscal year 2032, marking a major advancement in the exploration of primordial cosmology and fundamental physics. Orbiting the Sun-Earth Lagrangian point L2, this JAXA-led strategic L-class mission will conduct a comprehensive mapping of the CMB polarization across the entire sky. During its 3-year mission, LiteBIRD will employ three telescopes within 15 unique frequency bands (ranging from 34 through 448 GHz), targeting a sensitivity of 2.2\,$\mu$K-arcmin and a resolution of 0.5$^\circ$ at 100\,GHz. Its primary goal is to measure the tensor-to-scalar ratio $r$ with an uncertainty $\delta r = 0.001$, including systematic errors and margin. If $r \geq 0.01$, LiteBIRD expects to achieve a $>5\sigma$ detection in the $\ell=$2-10 and $\ell=$11-200 ranges separately, providing crucial insight into the early Universe. We describe LiteBIRD's scientific objectives, the application of systems engineering to mission requirements, the anticipated scientific impact, and the operations and scanning strategies vital to minimizing systematic effects. We will also highlight LiteBIRD's synergies with concurrent CMB projects., Comment: 23 pages, 9 figures, 1 table, SPIE Astronomical Telescopes + Instrumentation 2024

Published
2024

4. Probing Cosmic Inflation with the LiteBIRD Cosmic Microwave Background Polarization Survey

Author

LiteBIRD Collaboration, Allys, E., Arnold, K., Aumont, J., Aurlien, R., Azzoni, S., Baccigalupi, C., Banday, A. J., Banerji, R., Barreiro, R. B., Bartolo, N., Bautista, L., Beck, D., Beckman, S., Bersanelli, M., Boulanger, F., Brilenkov, M., Bucher, M., Calabrese, E., Campeti, P., Carones, A., Casas, F. J., Catalano, A., Chan, V., Cheung, K., Chinone, Y., Clark, S. E., Columbro, F., D'Alessandro, G., de Bernardis, P., de Haan, T., de la Hoz, E., De Petris, M., Della Torre, S., Diego-Palazuelos, P., Dobbs, M., Dotani, T., Duval, J. M., Elleflot, T., Eriksen, H. K., Errard, J., Essinger-Hileman, T., Finelli, F., Flauger, R., Franceschet, C., Fuskeland, U., Galloway, M., Ganga, K., Gerbino, M., Gervasi, M., Génova-Santos, R. T., Ghigna, T., Giardiello, S., Gjerløw, E., Grain, J., Grupp, F., Gruppuso, A., Gudmundsson, J. E., Halverson, N. W., Hargrave, P., Hasebe, T., Hasegawa, M., Hazumi, M., Henrot-Versillé, S., Hensley, B., Hergt, L. T., Herman, D., Hivon, E., Hlozek, R. A., Hornsby, A. L., Hoshino, Y., Hubmayr, J., Ichiki, K., Iida, T., Imada, H., Ishino, H., Jaehnig, G., Katayama, N., Kato, A., Keskitalo, R., Kisner, T., Kobayashi, Y., Kogut, A., Kohri, K., Komatsu, E., Komatsu, K., Konishi, K., Krachmalnicoff, N., Kuo, C. L., Lamagna, L., Lattanzi, M., Lee, A. T., Leloup, C., Levrier, F., Linder, E., Luzzi, G., Macias-Perez, J., Maciaszek, T., Maffei, B., Maino, D., Mandelli, S., Martínez-González, E., Masi, S., Massa, M., Matarrese, S., Matsuda, F. T., Matsumura, T., Mele, L., Migliaccio, M., Minami, Y., Moggi, A., Montgomery, J., Montier, L., Morgante, G., Mot, B., Nagano, Y., Nagasaki, T., Nagata, R., Nakano, R., Namikawa, T., Nati, F., Natoli, P., Nerval, S., Noviello, F., Odagiri, K., Oguri, S., Ohsaki, H., Pagano, L., Paiella, A., Paoletti, D., Passerini, A., Patanchon, G., Piacentini, F., Piat, M., Pisano, G., Polenta, G., Poletti, D., Prouvé, T., Puglisi, G., Rambaud, D., Raum, C., Realini, S., Reinecke, M., Remazeilles, M., Ritacco, A., Roudil, G., Rubino-Martin, J. A., Russell, M., Sakurai, H., Sakurai, Y., Sasaki, M., Scott, D., Sekimoto, Y., Shinozaki, K., Shiraishi, M., Shirron, P., Signorelli, G., Spinella, F., Stever, S., Stompor, R., Sugiyama, S., Sullivan, R. M., Suzuki, A., Svalheim, T. L., Switzer, E., Takaku, R., Takakura, H., Takase, Y., Tartari, A., Terao, Y., Thermeau, J., Thommesen, H., Thompson, K. L., Tomasi, M., Tominaga, M., Tristram, M., Tsuji, M., Tsujimoto, M., Vacher, L., Vielva, P., Vittorio, N., Wang, W., Watanuki, K., Wehus, I. K., Weller, J., Westbrook, B., Wilms, J., Winter, B., Wollack, E. J., Yumoto, J., and Zannoni, M.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
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$\mu$K-arcmin, with a typical angular resolution of 0.5$^\circ$ 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., Comment: 155 pages, accepted for publication in PTEP

Published
2022
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5. Superclustering with the Atacama Cosmology Telescope and Dark Energy Survey. I. Evidence for Thermal Energy Anisotropy Using Oriented Stacking

Author

Lokken, M, Hložek, R, van Engelen, A, Madhavacheril, M, Baxter, E, DeRose, J, Doux, C, Pandey, S, Rykoff, ES, Stein, G, To, C, Abbott, TMC, Adhikari, S, Aguena, M, Allam, S, Andrade-Oliveira, F, Annis, J, Battaglia, N, Bernstein, GM, Bertin, E, Bond, JR, Brooks, D, Calabrese, E, Rosell, A Carnero, Kind, M Carrasco, Carretero, J, Cawthon, R, Choi, A, Costanzi, M, Crocce, M, da Costa, LN, da Silva Pereira, ME, De Vicente, J, Desai, S, Dietrich, JP, Doel, P, Dunkley, J, Everett, S, Evrard, AE, Ferraro, S, Flaugher, B, Fosalba, P, Frieman, J, Gallardo, PA, García-Bellido, J, Gaztanaga, E, Gerdes, DW, Giannantonio, T, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Hill, JC, Hilton, M, Hincks, AD, Hinton, SR, Hollowood, DL, Honscheid, K, Hoyle, B, Huang, Z, Hughes, JP, Huterer, D, Jain, B, James, DJ, Jeltema, T, Kuehn, K, Lima, M, Maia, MAG, Marshall, JL, McMahon, J, Melchior, P, Menanteau, F, Miquel, R, Mohr, JJ, Moodley, K, Morgan, R, Nati, F, Page, L, Ogando, RLC, Palmese, A, Paz-Chinchón, F, Malagón, AA Plazas, Pieres, A, Romer, AK, Rozo, E, Sanchez, E, Scarpine, V, Schillaci, A, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, Sheldon, E, Shin, T, Sifón, C, Smith, M, Soares-Santos, M, Suchyta, E, Swanson, MEC, Tarle, G, and Thomas, D

Subjects
Nuclear and Plasma Physics, Physical Sciences, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

The cosmic web contains filamentary structure on a wide range of scales. On the largest scales, superclustering aligns multiple galaxy clusters along intercluster bridges, visible through their thermal Sunyaev-Zel'dovich signal in the cosmic microwave background. We demonstrate a new, flexible method to analyze the hot gas signal from multiscale extended structures. We use a Compton y-map from the Atacama Cosmology Telescope (ACT) stacked on redMaPPer cluster positions from the optical Dark Energy Survey (DES). Cutout images from the y-map are oriented with large-scale structure information from DES galaxy data such that the superclustering signal is aligned before being overlaid. We find evidence of an extended quadrupole moment of the stacked y signal at the 3.5σ level, demonstrating that the large-scale thermal energy surrounding galaxy clusters is anisotropically distributed. We compare our ACT × DES results with the Buzzard simulations, finding broad agreement. Using simulations, we highlight the promise of this novel technique for constraining the evolution of anisotropic, non-Gaussian structure using future combinations of microwave and optical surveys.

Published
2022

6. SNIa-Cosmology Analysis Results from Simulated LSST Images: from Difference Imaging to Constraints on Dark Energy

Author

Sánchez, B., Kessler, R., Scolnic, D., Armstrong, B., Biswas, R., Bogart, J., Chiang, J., Cohen-Tanugi, J., Fouchez, D., Gris, Ph., Heitmann, K., Hložek, R., Jha, S., Kelly, H., Liu, S., Narayan, G., Racine, B., Rykoff, E., Sullivan, M., Walter, C., Wood-Vasey, M., and Collaboration, The LSST Dark Energy Science

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

The Vera Rubin Observatory Legacy Survey of Space and Time (LSST) is expected to process ${\sim}10^6$ transient detections per night. For precision measurements of cosmological parameters and rates, it is critical to understand the detection efficiency, magnitude limits, artifact contamination levels, and biases in the selection and photometry. Here we rigorously test the LSST Difference Image Analysis (DIA) pipeline using simulated images from the Rubin Observatory LSST Dark Energy Science Collaboration (DESC) Data Challenge (DC2) simulation for the Wide-Fast-Deep (WFD) survey area. DC2 is the first large-scale (300 deg$^2$) image simulation of a transient survey that includes realistic cadence, variable observing conditions, and CCD image artifacts. We analyze ${\sim}$15 deg$^2$ of DC2 over a 5-year time-span in which artificial point-sources from Type Ia Supernovae (SNIa) light curves have been overlaid onto the images. We measure the detection efficiency as a function of Signal-to-Noise Ratio (SNR) and find a $50\%$ efficiency at $\rm{SNR}=5.8$. The magnitude limits for each filter are: $u=23.66$, $g=24.69$, $r=24.06$, $i=23.45$, $z=22.54$, $y=21.62$ $\rm{mag}$. The artifact contamination is $\sim90\%$ of detections, corresponding to $\sim1000$ artifacts/deg$^2$ in $g$ band, and falling to 300 per deg$^2$ in $y$ band. The photometry has biases $<1\%$ for magnitudes $19.5 < m <23$. Our DIA performance on simulated images is similar to that of the Dark Energy Survey pipeline applied to real images. We also characterize DC2 image properties to produce catalog-level simulations needed for distance bias corrections. We find good agreement between DC2 data and simulations for distributions of SNR, redshift, and fitted light-curve properties. Applying a realistic SNIa-cosmology analysis for redshifts $z<1$, we recover the input cosmology parameters to within statistical uncertainties., Comment: Submitting to Astronomy & Astrophysics

Published
2021
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7. 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

8. 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

9. SNIa Cosmology Analysis Results from Simulated LSST Images: From Difference Imaging to Constraints on Dark Energy

Author

Sánchez, B. O., primary, Kessler, R., additional, Scolnic, D., additional, Armstrong, R., additional, Biswas, R., additional, Bogart, J., additional, Chiang, J., additional, Cohen-Tanugi, J., additional, Fouchez, D., additional, Gris, Ph., additional, Heitmann, K., additional, Hložek, R., additional, Jha, S., additional, Kelly, H., additional, Liu, S., additional, Narayan, G., additional, Racine, B., additional, Rykoff, E., additional, Sullivan, M., additional, Walter, C. W., additional, and Wood-Vasey, W. M., additional

Published
2022
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10. SNIa Cosmology Analysis Results from Simulated LSST Images : From Difference Imaging to Constraints on Dark Energy

Author

Sanchez, B. O., Kessler, R., Scolnic, D., Armstrong, R., Biswas, Rahul, Bogart, J., Chiang, J., Cohen-Tanugi, J., Fouchez, D., Gris, Ph., Heitmann, K., Hložek, R., Jha, S., Kelly, H., Liu, S., Narayan, G., Racine, B., Rykoff, E., Sullivan, M., Walter, C. W., Wood-Vasey, W. M., Sanchez, B. O., Kessler, R., Scolnic, D., Armstrong, R., Biswas, Rahul, Bogart, J., Chiang, J., Cohen-Tanugi, J., Fouchez, D., Gris, Ph., Heitmann, K., Hložek, R., Jha, S., Kelly, H., Liu, S., Narayan, G., Racine, B., Rykoff, E., Sullivan, M., Walter, C. W., and Wood-Vasey, W. M.

Abstract

The Vera Rubin Observatory Legacy Survey of Space and Time (LSST) is expected to process ∼106 transient detections per night. For precision measurements of cosmological parameters and rates, it is critical to understand the detection efficiency, magnitude limits, artifact contamination levels, and biases in the selection and photometry. Here we rigorously test the LSST Difference Image Analysis (DIA) pipeline using simulated images from the Rubin Observatory LSST Dark Energy Science Collaboration Data Challenge (DC2) simulation for the Wide-Fast-Deep survey area. DC2 is the first large-scale (300 deg2) image simulation of a transient survey that includes realistic cadence, variable observing conditions, and CCD image artifacts. We analyze ∼15 deg2 of DC2 over a 5 yr time span in which artificial point sources from Type Ia supernova (SNIa) light curves have been overlaid onto the images. The magnitude limits per filter are u = 23.66 mag, g = 24.69 mag, r = 24.06 mag, i = 23.45 mag, z = 22.54 mag, and y = 21.62 mag. The artifact contamination levels are ∼90% of all detections, corresponding to ∼1000 artifacts deg–2 in g band, and falling to 300 deg–2 in y band. The photometry has biases <1% for magnitudes 19.5 < m < 23. Our DIA performance on simulated images is similar to that of the Dark Energy Survey difference-imaging pipeline on real images. We also characterize DC2 image properties to produce catalog-level simulations needed for distance bias corrections. We find good agreement between DC2 data and simulations for distributions of signal-to-noise ratio, redshift, and fitted light-curve properties. Applying a realistic SNIa cosmology analysis for redshifts z < 1, we recover the input cosmology parameters to within statistical uncertainties.

Published
2022
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