Author: "Devlin, M" / Database: OAIster - Searchworks@Jio Institute Digital Library Search Results

Your search keyword '"Devlin, M"' showing total 343 results

Start Over Author "Devlin, M" Database OAIster

343 results on '"Devlin, M"'

1. 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

2. 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

3. The Atacama Cosmology Telescope: map-based noise simulations for DR6

Author: Atkins, Z, Duivenvoorden, A, Coulton, W, Qu, F, Aiola, S, Calabrese, E, Chesmore, G, Choi, S, Devlin, M, Dunkley, J, Hervias-Caimapo, C, Guan, Y, Posta, A, Li, Z, Louis, T, Madhavacheril, M, Moodley, K, Naess, S, Nati, F, Niemack, M, Page, L, Puddu, R, Salatino, M, Sifon, C, Staggs, S, Vargas, C, Vavagiakis, E, Wollack, E, Atkins Z., Duivenvoorden A. J., Coulton W. R., Qu F. J., Aiola S., Calabrese E., Chesmore G. E., Choi S. K., Devlin M. J., Dunkley J., Hervias-Caimapo C., Guan Y., Posta A. L., Li Z., Louis T., Madhavacheril M. S., Moodley K., Naess S., Nati F., Niemack M. D., Page L., Puddu R., Salatino M., Sifon C., Staggs S. T., Vargas C., Vavagiakis E. M., Wollack E. J., Atkins, Z, Duivenvoorden, A, Coulton, W, Qu, F, Aiola, S, Calabrese, E, Chesmore, G, Choi, S, Devlin, M, Dunkley, J, Hervias-Caimapo, C, Guan, Y, Posta, A, Li, Z, Louis, T, Madhavacheril, M, Moodley, K, Naess, S, Nati, F, Niemack, M, Page, L, Puddu, R, Salatino, M, Sifon, C, Staggs, S, Vargas, C, Vavagiakis, E, Wollack, E, Atkins Z., Duivenvoorden A. J., Coulton W. R., Qu F. J., Aiola S., Calabrese E., Chesmore G. E., Choi S. K., Devlin M. J., Dunkley J., Hervias-Caimapo C., Guan Y., Posta A. L., Li Z., Louis T., Madhavacheril M. S., Moodley K., Naess S., Nati F., Niemack M. D., Page L., Puddu R., Salatino M., Sifon C., Staggs S. T., Vargas C., Vavagiakis E. M., and Wollack E. J.
Abstract: The increasing statistical power of cosmic microwave background (CMB) datasets requires a commensurate effort in understanding their noise properties. The noise in maps from ground-based instruments is dominated by large-scale correlations, which poses a modeling challenge. This paper develops novel models of the complex noise covariance structure in the Atacama Cosmology Telescope Data Release 6 (ACT DR6) maps. We first enumerate the noise properties that arise from the combination of the atmosphere and the ACT scan strategy. We then prescribe a class of Gaussian, map-based noise models, including a new wavelet-based approach that uses directional wavelet kernels for modeling correlated instrumental noise. The models are empirical, whose only inputs are a small number of independent realizations of the same region of sky. We evaluate the performance of these models against the ACT DR6 data by drawing ensembles of noise realizations. Applying these simulations to the ACT DR6 power spectrum pipeline reveals a ∼ 20% excess in the covariance matrix diagonal when compared to an analytic expression that assumes noise properties are uniquely described by their power spectrum. Along with our public code, mnms, this work establishes a necessary element in the science pipelines of both ACT DR6 and future ground-based CMB experiments such as the Simons Observatory (SO).
Published: 2023

4. The Simons Observatory: A large-diameter truss for a refracting telescope cooled to 1 K

Author: Crowley, K, Dow, P, Shroyer, J, Groh, J, Dober, B, Spisak, J, Galitzki, N, Bhandarkar, T, Devlin, M, Dicker, S, Gallardo, P, Harrington, K, Iuliano, J, Johnson, B, Johnson, D, Kofman, A, Kusaka, A, Lee, A, Limon, M, Nati, F, Orlowski-Scherer, J, Page, L, Randall, M, Teply, G, Tsan, T, Wollack, E, Xu, Z, Zhu, N, Crowley K. D., Dow P., Shroyer J. E., Groh J. C., Dober B., Spisak J., Galitzki N., Bhandarkar T., Devlin M. J., Dicker S., Gallardo P. A., Harrington K., Iuliano J., Johnson B. R., Johnson D., Kofman A. M., Kusaka A., Lee A., Limon M., Nati F., Orlowski-Scherer J., Page L., Randall M., Teply G., Tsan T., Wollack E. J., Xu Z., Zhu N., Crowley, K, Dow, P, Shroyer, J, Groh, J, Dober, B, Spisak, J, Galitzki, N, Bhandarkar, T, Devlin, M, Dicker, S, Gallardo, P, Harrington, K, Iuliano, J, Johnson, B, Johnson, D, Kofman, A, Kusaka, A, Lee, A, Limon, M, Nati, F, Orlowski-Scherer, J, Page, L, Randall, M, Teply, G, Tsan, T, Wollack, E, Xu, Z, Zhu, N, Crowley K. D., Dow P., Shroyer J. E., Groh J. C., Dober B., Spisak J., Galitzki N., Bhandarkar T., Devlin M. J., Dicker S., Gallardo P. A., Harrington K., Iuliano J., Johnson B. R., Johnson D., Kofman A. M., Kusaka A., Lee A., Limon M., Nati F., Orlowski-Scherer J., Page L., Randall M., Teply G., Tsan T., Wollack E. J., Xu Z., and Zhu N.
Abstract: We present the design and measured performance of a new carbon fiber strut design that is used in a cryogenically cooled truss for the Simons Observatory small aperture telescope. The truss consists of two aluminum 6061 rings separated by 24 struts. Each strut consists of a central carbon fiber tube fitted with two aluminum end caps. We tested the performance of the strut and truss by (i) cryogenically cycling and destructively pull-Testing strut samples, (ii) non-destructively pull-Testing the final truss, and (iii) measuring the thermal conductivity of the carbon fiber tubes. We found that the strut strength is limited by the mounting fasteners and the strut end caps, not the epoxy adhesive or the carbon fiber tube. This result is consistent with our numerical predictions. Our thermal measurements suggest that the conductive heat load through the struts (from 4 to 1 K) will be less than 1 mW. This strut design may be a promising candidate for use in other cryogenic support structures.
Published: 2022

5. Templates of expected measurement uncertainties for average prompt and total fission neutron multiplicities

Author: Neudecker, D., Carlson, A.D., Croft, S., Devlin, M., Kelly, K.J., Lovell, A.E., Marini, P., Taieb, J., Neudecker, D., Carlson, A.D., Croft, S., Devlin, M., Kelly, K.J., Lovell, A.E., Marini, P., and Taieb, J.
Abstract: In this paper, we provide templates of measurement uncertainty sources expected to appear for average prompt- and total-fission neutron multiplicities, and , for the following measurement types: absolute manganese-bath experiments for , absolute and ratio liquid-scintillator measurements for . These templates also suggest a typical range of these uncertainties and their correlations based on a survey of available experimental data, associated literature, and feedback from experimentalists. In addition, the information needed to faithfully include the associated experimental data into the nuclear-data evaluation process is provided.
Published: 2023

6. XLSSC 122 caught in the act of growing up: Spatially resolved SZ observations of a z=1.98 galaxy cluster

Author: van Marrewijk, J., Di Mascolo, L., Gill, A. S., Battaglia, N., Battistelli, E. S., Bond, J. R., Devlin, M. J., Doze, P., Dunkley, J., Knowles, K., Hincks, A., Hughes, J. P., Hilton, M., Moodley, K., Mroczkowski, T., Naess, S., Partridge, B., Popping, G., Sifón, C., Staggs, S. T., Wollack, E. J., van Marrewijk, J., Di Mascolo, L., Gill, A. S., Battaglia, N., Battistelli, E. S., Bond, J. R., Devlin, M. J., Doze, P., Dunkley, J., Knowles, K., Hincks, A., Hughes, J. P., Hilton, M., Moodley, K., Mroczkowski, T., Naess, S., Partridge, B., Popping, G., Sifón, C., Staggs, S. T., and Wollack, E. J.
Abstract: How protoclusters evolved from sparse galaxy overdensities to mature galaxy clusters is still not well understood. In this context, detecting and characterizing the hot ICM at high redshifts (z~2) is key to understanding how the continuous accretion from and mergers along the filamentary large-scale structure impact the first phases of cluster formation. We study the dynamical state and morphology of the z=1.98 galaxy cluster XLSSC 122 with high-resolution observations (~5") of the ICM through the SZ effect. Via Bayesian forward modeling, we map the ICM on scales from the virial radius down to the core of the cluster. To constrain such a broad range of spatial scales, we employ a new technique that jointly forward-models parametric descriptions of the pressure distribution to interferometric ACA and ALMA observations and multi-band imaging data from the 6-m, single-dish Atacama Cosmology Telescope. We detect the SZ effect with $11\sigma$ in the ALMA+ACA observations and find a flattened inner pressure profile that is consistent with a non-cool core classification with a significance of $>3\sigma$. In contrast to the previous works, we find better agreement between the SZ effect signal and the X-ray emission as well as the cluster member distribution. Further, XLSSC 122 exhibits an excess of SZ flux in the south of the cluster where no X-ray emission is detected. By reconstructing the interferometric observations and modeling in the uv-plane, we obtain a tentative detection of an infalling group or filamentary-like structure that is believed to boost and heat up the ICM while the density of the gas is low. In addition, we provide an improved SZ mass of $M_{500,\mathrm{c}} = 1.66^{+0.23}_{-0.20} \times 10^{14} \rm M_\odot$. Altogether, the observations indicate that we see XLSSC 122 in a dynamic phase of cluster formation while a large reservoir of gas is already thermalized.
Published: 2023

7. Cosmological shocks around galaxy clusters: A coherent investigation with DES, SPT & ACT

Author: Anbajagane, D., Chang, C., Baxter, E. J., Charney, S., Lokken, M., Aguena, M., Allam, S., Alves, O., Amon, A., An, R., Andrade-Oliveira, F., Bacon, D., Battaglia, N., Bechtol, K., Becker, M. R., Benson, B. A., Bernstein, G. M., Bleem, L., Bocquet, S., Bond, J. R., Brooks, D., Rosell, A. Carnero, Kind, M. Carrasco, Chen, R., Choi, A., Costanzi, M., Crawford, T. M., Crocce, M., da Costa, L. N., Pereira, M. E. S., Davis, T. M., De Vicente, J., Desai, S., Devlin, M. J., Diehl, H. T., Doel, P., Doux, C., Drlica-Wagner, A., Elvin-Poole, J., Ferrero, I., Ferte, A., Flaugher, B., Fosalba, P., Friedel, D., Frieman, J., Garcia-Bellido, J., Gatti, M., Giannini, G., Grandis, S., Gruen, D., Gruendl, R. A., Gutierrez, G., Harrison, I., Hill, J. C., Hilton, M., Hinton, S. R., Hollowood, D. L., Honscheid, K., Jain, B., James, D. J., Jarvis, M., Kuehn, K., Lin, M., MacCrann, N., Marshall, J. L., McCullough, J., McMahon, J. J., Mena-Fernandez, J., Menanteau, F., Miquel, R., Moodley, K., Mroczkowski, T., Myles, J., Naess, S., Navarro-Alsina, A., Ogando, R. L. C., Page, L. A., Palmese, A., Pandey, S., Patridge, B., Pieres, A., Malagon, A. A. Plazas, Porredon, A., Prat, J., Reichardt, C., Reil, K., Rodriguez-Monroy, M., Rollins, R. P., Romer, A. K., Rykoff, E. S., Sanchez, E., Sanchez, C., Cid, D. Sanchez, Schaan, E., Schubnell, M., Secco, L. F., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Sifon, C., Smith, M., Staggs, S. T., Suchyta, E., Swanson, M. E. C., Tarle, G., To, C., Troxel, M. A., Tutusaus, I., Vavagiakis, E. M., Weaverdyck, N., Weller, J., Wiseman, P., Wollack, E. J., Yanny, B., Anbajagane, D., Chang, C., Baxter, E. J., Charney, S., Lokken, M., Aguena, M., Allam, S., Alves, O., Amon, A., An, R., Andrade-Oliveira, F., Bacon, D., Battaglia, N., Bechtol, K., Becker, M. R., Benson, B. A., Bernstein, G. M., Bleem, L., Bocquet, S., Bond, J. R., Brooks, D., Rosell, A. Carnero, Kind, M. Carrasco, Chen, R., Choi, A., Costanzi, M., Crawford, T. M., Crocce, M., da Costa, L. N., Pereira, M. E. S., Davis, T. M., De Vicente, J., Desai, S., Devlin, M. J., Diehl, H. T., Doel, P., Doux, C., Drlica-Wagner, A., Elvin-Poole, J., Ferrero, I., Ferte, A., Flaugher, B., Fosalba, P., Friedel, D., Frieman, J., Garcia-Bellido, J., Gatti, M., Giannini, G., Grandis, S., Gruen, D., Gruendl, R. A., Gutierrez, G., Harrison, I., Hill, J. C., Hilton, M., Hinton, S. R., Hollowood, D. L., Honscheid, K., Jain, B., James, D. J., Jarvis, M., Kuehn, K., Lin, M., MacCrann, N., Marshall, J. L., McCullough, J., McMahon, J. J., Mena-Fernandez, J., Menanteau, F., Miquel, R., Moodley, K., Mroczkowski, T., Myles, J., Naess, S., Navarro-Alsina, A., Ogando, R. L. C., Page, L. A., Palmese, A., Pandey, S., Patridge, B., Pieres, A., Malagon, A. A. Plazas, Porredon, A., Prat, J., Reichardt, C., Reil, K., Rodriguez-Monroy, M., Rollins, R. P., Romer, A. K., Rykoff, E. S., Sanchez, E., Sanchez, C., Cid, D. Sanchez, Schaan, E., Schubnell, M., Secco, L. F., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Sifon, C., Smith, M., Staggs, S. T., Suchyta, E., Swanson, M. E. C., Tarle, G., To, C., Troxel, M. A., Tutusaus, I., Vavagiakis, E. M., Weaverdyck, N., Weller, J., Wiseman, P., Wollack, E. J., and Yanny, B.
Abstract: We search for signatures of cosmological shocks in gas pressure profiles of galaxy clusters using the cluster catalogs from three surveys: the Dark Energy Survey (DES) Year 3, the South Pole Telescope (SPT) SZ survey, and the Atacama Cosmology Telescope (ACT) data releases 4, 5, and 6, and using thermal Sunyaev-Zeldovich (SZ) maps from SPT and ACT. The combined cluster sample contains around $10^5$ clusters with mass and redshift ranges $10^{13.7} < M_{\rm 200m}/M_\odot < 10^{15.5}$ and $0.1 < z < 2$, and the total sky coverage of the maps is $\approx 15,000 \,\,{\rm deg}^2$. We find a clear pressure deficit at $R/R_{\rm 200m}\approx 1.1$ in SZ profiles around both ACT and SPT clusters, estimated at $6\sigma$ significance, which is qualitatively consistent with a shock-induced thermal non-equilibrium between electrons and ions. The feature is not as clearly determined in profiles around DES clusters. We verify that measurements using SPT or ACT maps are consistent across all scales, including in the deficit feature. The SZ profiles of optically selected and SZ-selected clusters are also consistent for higher mass clusters. Those of less massive, optically selected clusters are suppressed on small scales by factors of 2-5 compared to predictions, and we discuss possible interpretations of this behavior. An oriented stacking of clusters -- where the orientation is inferred from the SZ image, the brightest cluster galaxy, or the surrounding large-scale structure measured using galaxy catalogs -- shows the normalization of the one-halo and two-halo terms vary with orientation. Finally, the location of the pressure deficit feature is statistically consistent with existing estimates of the splashback radius., Comment: [v2]: Version accepted to MNRAS
Published: 2023

8. Cosmology from Cross-Correlation of ACT-DR4 CMB Lensing and DES-Y3 Cosmic Shear

Author: Shaikh, S., Harrison, I., van Engelen, A., Marques, G. A., Abbott, T. M. C., Aguena, M., Alves, O., Amon, A., An, R., Bacon, D., Battaglia, N., Becker, M. R., Bernstein, G. M., Bertin, E., Blazek, J., Bond, J. R., Brooks, D., Burke, D. L., Calabrese, E., Rosell, A. Carnero, Carretero, J., Cawthon, R., Chang, C., Chen, R., Choi, A., Choi, S. K., da Costa, L. N., Pereira, M. E. S., Darwish, O., Davis, T. M., Desai, S., Devlin, M., Diehl, H. T., Doel, P., Doux, C., Elvin-Poole, J., Farren, G. S., Ferraro, S., Ferrero, I., Ferté, A., Flaugher, B., Frieman, J., Gatti, M., Giannini, G., Giardiello, S., Gruen, D., Gruendl, R. A., Gutierrez, G., Hill, J. C., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huffenberger, K. M., Huterer, D., James, D. J., Jarvis, M., Jeffrey, N., Jense, H. T., Knowles, K., Kim, J., Kramer, D., Lahav, O., Lee, S., Lima, M., MacCrann, N., Madhavacheril, M. S., Marshall, J. L., McCullough, J., Mehta, Y., Mena-Fernández, J., Miquel, R., Mohr, J. J., Moodley, K., Myles, J., Navarro-Alsina, A., Newburgh, L., Niemack, M. D., Omori, Y., Pandey, S., Partridge, B., Pieres, A., Malagón, A. A. Plazas, Porredon, A., Prat, J., Qu, F. J., Robertson, N., Rollins, R. P., Roodman, A., Samuroff, S., Sánchez, C., Sanchez, E., Cid, D. Sanchez, Secco, L. F., Sehgal, N., Sheldon, E., Sherwin, B. D., Shin, T., Smith, C. Sifón M., Suchyta, E., Swanson, M. E. C., Tarle, G., Troxel, M. A., Tutusaus, I., Vargas, C., Weaverdyck, N., Wiseman, P., Yamamoto, M., Zuntz, J., Shaikh, S., Harrison, I., van Engelen, A., Marques, G. A., Abbott, T. M. C., Aguena, M., Alves, O., Amon, A., An, R., Bacon, D., Battaglia, N., Becker, M. R., Bernstein, G. M., Bertin, E., Blazek, J., Bond, J. R., Brooks, D., Burke, D. L., Calabrese, E., Rosell, A. Carnero, Carretero, J., Cawthon, R., Chang, C., Chen, R., Choi, A., Choi, S. K., da Costa, L. N., Pereira, M. E. S., Darwish, O., Davis, T. M., Desai, S., Devlin, M., Diehl, H. T., Doel, P., Doux, C., Elvin-Poole, J., Farren, G. S., Ferraro, S., Ferrero, I., Ferté, A., Flaugher, B., Frieman, J., Gatti, M., Giannini, G., Giardiello, S., Gruen, D., Gruendl, R. A., Gutierrez, G., Hill, J. C., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huffenberger, K. M., Huterer, D., James, D. J., Jarvis, M., Jeffrey, N., Jense, H. T., Knowles, K., Kim, J., Kramer, D., Lahav, O., Lee, S., Lima, M., MacCrann, N., Madhavacheril, M. S., Marshall, J. L., McCullough, J., Mehta, Y., Mena-Fernández, J., Miquel, R., Mohr, J. J., Moodley, K., Myles, J., Navarro-Alsina, A., Newburgh, L., Niemack, M. D., Omori, Y., Pandey, S., Partridge, B., Pieres, A., Malagón, A. A. Plazas, Porredon, A., Prat, J., Qu, F. J., Robertson, N., Rollins, R. P., Roodman, A., Samuroff, S., Sánchez, C., Sanchez, E., Cid, D. Sanchez, Secco, L. F., Sehgal, N., Sheldon, E., Sherwin, B. D., Shin, T., Smith, C. Sifón M., Suchyta, E., Swanson, M. E. C., Tarle, G., Troxel, M. A., Tutusaus, I., Vargas, C., Weaverdyck, N., Wiseman, P., Yamamoto, M., and Zuntz, J.
Abstract: Cross-correlation between weak lensing of the Cosmic Microwave Background (CMB) and weak lensing of galaxies offers a way to place robust constraints on cosmological and astrophysical parameters with reduced sensitivity to certain systematic effects affecting individual surveys. We measure the angular cross-power spectrum between the Atacama Cosmology Telescope (ACT) DR4 CMB lensing and the galaxy weak lensing measured by the Dark Energy Survey (DES) Y3 data. Our baseline analysis uses the CMB convergence map derived from ACT-DR4 and $\textit{Planck}$ data, where most of the contamination due to the thermal Sunyaev Zel'dovich effect is removed, thus avoiding important systematics in the cross-correlation. In our modelling, we consider the nuisance parameters of the photometric uncertainty, multiplicative shear bias and intrinsic alignment of galaxies. The resulting cross-power spectrum has a signal-to-noise ratio $= 7.1$ and passes a set of null tests. We use it to infer the amplitude of the fluctuations in the matter distribution ($S_8 \equiv \sigma_8 (\Omega_{\rm m}/0.3)^{0.5} = 0.782\pm 0.059$) with informative but well-motivated priors on the nuisance parameters. We also investigate the validity of these priors by significantly relaxing them and checking the consistency of the resulting posteriors, finding them consistent, albeit only with relatively weak constraints. This cross-correlation measurement will improve significantly with the new ACT-DR6 lensing map and form a key component of the joint 6x2pt analysis between DES and ACT., Comment: 26 pages, 30 figures (including appendices). Data associated with this article is available at https://github.com/itrharrison/actdr4kappa-x-desy3gamma-data
Published: 2023

9. Witnessing the intracluster medium assembly at the cosmic noon in JKCS041

Author: Andreon, S., Romero, C., Aussel, H., Bhandarkar, T., Devlin, M., Dicker, S., Ladjelate, B., Lowe, I., Mason, B., Mroczkowski, T., Raichoor, A., Sarazin, C., Trinchieri, G., Andreon, S., Romero, C., Aussel, H., Bhandarkar, T., Devlin, M., Dicker, S., Ladjelate, B., Lowe, I., Mason, B., Mroczkowski, T., Raichoor, A., Sarazin, C., and Trinchieri, G.
Abstract: In this work we study the intracluster medium of a galaxy cluster at the cosmic noon: JKCS041 at z=1.803. A 28h long Sunyaev-Zel'dovich (SZ) observation using MUSTANG-2 allows us to detect JKCS041, even if intrinsically extremely faint compared to other SZ-detected clusters. We found that the SZ peak is offset from the X-ray center by about 220 kpc in the direction of the brightest cluster galaxy, which we interpret as due to the cluster being observed just after first passage of a major merger. JKCS041 has a low central pressure and a low Compton Y compared to local clusters selected by their intracluster medium (ICM), likely because the cluster is still in the process of assembly but also in part because of a hard-to-quantify bias in current local ICM-selected samples. JKCS041 has a 0.5 dex fainter Y signal than another less massive z~1.8 cluster, exemplifying how much different weak-lensing mass and SZ mass can be at high redshift. The observations we present provide us with the measurement of the most distant resolved pressure profile of a galaxy cluster. Comparison with a library of plausibly descendants shows that JKCS041 pressure profile will likely increase by about 0.7 dex in the next 10 Gyr at all radii., Comment: MNRAS, in press
Published: 2023
Full Text: View/download PDF

10. The Atacama Cosmology Telescope: Systematic Transient Search of 3 Day Maps

Author: Li, Y, Biermann, E, Naess, S, Aiola, S, An, R, Battaglia, N, Bhandarkar, T, Calabrese, E, Choi, S, Crowley, K, Devlin, M, Duell, C, Duff, S, Dunkley, J, Dünner, R, Gallardo, P, Guan, Y, Hervias-Caimapo, C, Hincks, A, Hubmayr, J, Huffenberger, K, Hughes, J, Kosowsky, A, Louis, T, Mallaby-Kay, M, Mcmahon, J, Nati, F, Niemack, M, Orlowski-Scherer, J, Page, L, Salatino, M, Sifón, C, Staggs, S, Vargas, C, Vavagiakis, E, Wang, Y, Wollack, E, Li, YQ, Choi, SK, Crowley, KT, Duell, CJ, Duff, SM, Gallardo, PA, Guan, YL, Hincks, AD, Huffenberger, KM, Hughes, JP, Niemack, MD, Staggs, ST, Vavagiakis, EM, Wang, YH, Wollack, EJ, Li, Y, Biermann, E, Naess, S, Aiola, S, An, R, Battaglia, N, Bhandarkar, T, Calabrese, E, Choi, S, Crowley, K, Devlin, M, Duell, C, Duff, S, Dunkley, J, Dünner, R, Gallardo, P, Guan, Y, Hervias-Caimapo, C, Hincks, A, Hubmayr, J, Huffenberger, K, Hughes, J, Kosowsky, A, Louis, T, Mallaby-Kay, M, Mcmahon, J, Nati, F, Niemack, M, Orlowski-Scherer, J, Page, L, Salatino, M, Sifón, C, Staggs, S, Vargas, C, Vavagiakis, E, Wang, Y, Wollack, E, Li, YQ, Choi, SK, Crowley, KT, Duell, CJ, Duff, SM, Gallardo, PA, Guan, YL, Hincks, AD, Huffenberger, KM, Hughes, JP, Niemack, MD, Staggs, ST, Vavagiakis, EM, Wang, YH, and Wollack, EJ
Abstract: We conduct a systematic search for transients in 3 yr of data (2017-2019) from the Atacama Cosmology Telescope (ACT). ACT covers 40% of the sky at three bands spanning from 77-277 GHz. Analysis of 3 day mean-subtracted sky maps, which were match filtered for point sources, yielded 29 transient detections. Eight of these transients are due to known asteroids, and three others were previously published. Four of these events occur in areas with poor noise models and thus we cannot be confident they are real transients. We are left with 14 new transient events occurring at 11 unique locations. All of these events are associated with either rotationally variable stars or cool stars. Ten events have flat or falling spectra indicating radiation from synchrotron emission. One event has a rising spectrum indicating a different engine for the flare.
Published: 2023

11. The atacama cosmology telescope: A catalog of >4000 Sunyaev–Zel’dovich galaxy clusters

Author: Hilton, M, Sifon, C, Naess, S, Madhavacheril, M, Oguri, M, Rozo, E, Rykoff, E, Adhikari, S, Aguena, M, Aiola, S, Allam, S, Amodeo, S, Amon, A, Annis, J, Ansarinejad, B, Abbott, T, Aros-Bunster, C, Austermann, J, Avila, S, Bacon, D, Battaglia, N, Beall, J, Becker, D, Bernstein, G, Bertin, E, Bhandarkar, T, Bhargava, S, Bond, J, Brooks, D, Burke, D, Calabrese, E, Carrasco Kind, M, Carretero, J, Choi, S, Choi, A, Conselice, C, Da Costa, L, Costanzi, M, Crichton, D, Crowley, K, Dunner, R, Denison, E, Devlin, M, Dicker, S, Diehl, H, Dietrich, J, Doel, P, Duff, S, Duivenvoorden, A, Dunkley, J, Everett, S, Ferraro, S, Ferte, A, Flaugher, B, Frieman, J, Ferrero, I, Gallardo, P, Garcia-Bellido, J, Gaztanaga, E, Giles, P, Golec, J, Gralla, M, Grandis, S, Gruen, D, Gerdes, D, Gruendl, R, Gschwend, J, Gutierrez, G, Han, D, Hartley, W, Hasselfield, M, Hill, J, Hilton, G, Hincks, A, Hinton, S, Ho, S, Honscheid, K, Hoyle, B, Hubmayr, J, Huffenberger, K, Hughes, J, Jaelani, A, Jain, B, James, D, Jeltema, T, Kent, S, Knowles, K, Koopman, B, Kuehn, K, Lahav, O, Lima, M, Lin, Y, Lokken, M, Loubser, S, Maccrann, N, Maia, M, Marriage, T, Martin, J, Mcmahon, J, Melchior, P, Menanteau, F, Miquel, R, Moodley, K, Morgan, R, Mroczkowski, T, Nati, F, Newburgh, L, Niemack, M, Nishizawa, A, Miyatake, H, Ogando, R, Orlowski-Scherer, J, Page, L, Palmese, A, Partridge, B, Paz-Chinchon, F, Phakathi, P, Plazas, A, Robertson, N, Romer, A, Carnero Rosell, A, Sanchez, E, Schaan, E, Schillaci, A, Sehgal, N, Serrano, S, Shin, T, Simon, S, Smith, M, Salatino, M, Soares-Santos, M, Spergel, D, Staggs, S, Storer, E, Suchyta, E, Swanson, M, Tarle, G, Thomas, D, To, C, Trac, H, Ullom, J, Vale, L, Van Lanen, J, Vavagiakis, E, De Vicente, J, Wilkinson, R, Wollack, E, Xu, Z, Zhan, Y, Hilton M., Sifon C., Naess S., Madhavacheril M., Oguri M., Rozo E., Rykoff E., Adhikari S., Aguena M., Aiola S., Allam S., Amodeo S., Amon A., Annis J., Ansarinejad B., Abbott T. M. C., Aros-Bunster C., Austermann J. E., Avila S., Bacon D., Battaglia N., Beall J. A., Becker D. T., Bernstein G. M., Bertin E., Bhandarkar T., Bhargava S., Bond J. R., Brooks D., Burke D. L., Calabrese E., Carrasco Kind M., Carretero J., Choi S. K., Choi A., Conselice C., Da Costa L. N., Costanzi M., Crichton D., Crowley K. T., Dunner R., Denison E. V., Devlin M. J., Dicker S. R., Diehl H. T., Dietrich J. P., Doel P., Duff S. M., Duivenvoorden A. J., Dunkley J., Everett S., Ferraro S., Ferte A., Flaugher B., Frieman J., Ferrero I., Gallardo P. A., Garcia-Bellido J., Gaztanaga E., Giles P., Golec J. E., Gralla M. B., Grandis S., Gruen D., Gerdes D. W., Gruendl R. A., Gschwend J., Gutierrez G., Han D., Hartley W. G., Hasselfield M., Hill J. C., Hilton G. C., Hincks A. D., Hinton S. R., Ho S. -P. P., Honscheid K., Hoyle B., Hubmayr J., Huffenberger K. M., Hughes J. P., Jaelani A. T., Jain B., James D. J., Jeltema T., Kent S., Knowles K., Koopman B. J., Kuehn K., Lahav O., Lima M., Lin Y. -T., Lokken M., Loubser S. I., MacCrann N., Maia M. A. G., Marriage T. A., Martin J., McMahon J., Melchior P., Menanteau F., Miquel R., Moodley K., Morgan R., Mroczkowski T., Nati F., Newburgh L. B., Niemack M. D., Nishizawa A. J., Miyatake H., Ogando R. L. C., Orlowski-Scherer J., Page L. A., Palmese A., Partridge B., Paz-Chinchon F., Phakathi P., Plazas A. A., Robertson N. C., Romer A. K., Carnero Rosell A., Sanchez E., Schaan E., Schillaci A., Sehgal N., Serrano S., Shin T., Simon S. M., Smith M., Salatino M., Soares-Santos M., Spergel D. N., Staggs S. T., Storer E. R., Suchyta E., Swanson M. E. C., Tarle G., Thomas D., To C., Trac H., Ullom J. N., Vale L. R., Van Lanen J., Vavagiakis E. M., De Vicente J., Wilkinson R. D., Wollack E. J., Xu Z., Zhan Y., Hilton, M, Sifon, C, Naess, S, Madhavacheril, M, Oguri, M, Rozo, E, Rykoff, E, Adhikari, S, Aguena, M, Aiola, S, Allam, S, Amodeo, S, Amon, A, Annis, J, Ansarinejad, B, Abbott, T, Aros-Bunster, C, Austermann, J, Avila, S, Bacon, D, Battaglia, N, Beall, J, Becker, D, Bernstein, G, Bertin, E, Bhandarkar, T, Bhargava, S, Bond, J, Brooks, D, Burke, D, Calabrese, E, Carrasco Kind, M, Carretero, J, Choi, S, Choi, A, Conselice, C, Da Costa, L, Costanzi, M, Crichton, D, Crowley, K, Dunner, R, Denison, E, Devlin, M, Dicker, S, Diehl, H, Dietrich, J, Doel, P, Duff, S, Duivenvoorden, A, Dunkley, J, Everett, S, Ferraro, S, Ferte, A, Flaugher, B, Frieman, J, Ferrero, I, Gallardo, P, Garcia-Bellido, J, Gaztanaga, E, Giles, P, Golec, J, Gralla, M, Grandis, S, Gruen, D, Gerdes, D, Gruendl, R, Gschwend, J, Gutierrez, G, Han, D, Hartley, W, Hasselfield, M, Hill, J, Hilton, G, Hincks, A, Hinton, S, Ho, S, Honscheid, K, Hoyle, B, Hubmayr, J, Huffenberger, K, Hughes, J, Jaelani, A, Jain, B, James, D, Jeltema, T, Kent, S, Knowles, K, Koopman, B, Kuehn, K, Lahav, O, Lima, M, Lin, Y, Lokken, M, Loubser, S, Maccrann, N, Maia, M, Marriage, T, Martin, J, Mcmahon, J, Melchior, P, Menanteau, F, Miquel, R, Moodley, K, Morgan, R, Mroczkowski, T, Nati, F, Newburgh, L, Niemack, M, Nishizawa, A, Miyatake, H, Ogando, R, Orlowski-Scherer, J, Page, L, Palmese, A, Partridge, B, Paz-Chinchon, F, Phakathi, P, Plazas, A, Robertson, N, Romer, A, Carnero Rosell, A, Sanchez, E, Schaan, E, Schillaci, A, Sehgal, N, Serrano, S, Shin, T, Simon, S, Smith, M, Salatino, M, Soares-Santos, M, Spergel, D, Staggs, S, Storer, E, Suchyta, E, Swanson, M, Tarle, G, Thomas, D, To, C, Trac, H, Ullom, J, Vale, L, Van Lanen, J, Vavagiakis, E, De Vicente, J, Wilkinson, R, Wollack, E, Xu, Z, Zhan, Y, Hilton M., Sifon C., Naess S., Madhavacheril M., Oguri M., Rozo E., Rykoff E., Adhikari S., Aguena M., Aiola S., Allam S., Amodeo S., Amon A., Annis J., Ansarinejad B., Abbott T. M. C., Aros-Bunster C., Austermann J. E., Avila S., Bacon D., Battaglia N., Beall J. A., Becker D. T., Bernstein G. M., Bertin E., Bhandarkar T., Bhargava S., Bond J. R., Brooks D., Burke D. L., Calabrese E., Carrasco Kind M., Carretero J., Choi S. K., Choi A., Conselice C., Da Costa L. N., Costanzi M., Crichton D., Crowley K. T., Dunner R., Denison E. V., Devlin M. J., Dicker S. R., Diehl H. T., Dietrich J. P., Doel P., Duff S. M., Duivenvoorden A. J., Dunkley J., Everett S., Ferraro S., Ferte A., Flaugher B., Frieman J., Ferrero I., Gallardo P. A., Garcia-Bellido J., Gaztanaga E., Giles P., Golec J. E., Gralla M. B., Grandis S., Gruen D., Gerdes D. W., Gruendl R. A., Gschwend J., Gutierrez G., Han D., Hartley W. G., Hasselfield M., Hill J. C., Hilton G. C., Hincks A. D., Hinton S. R., Ho S. -P. P., Honscheid K., Hoyle B., Hubmayr J., Huffenberger K. M., Hughes J. P., Jaelani A. T., Jain B., James D. J., Jeltema T., Kent S., Knowles K., Koopman B. J., Kuehn K., Lahav O., Lima M., Lin Y. -T., Lokken M., Loubser S. I., MacCrann N., Maia M. A. G., Marriage T. A., Martin J., McMahon J., Melchior P., Menanteau F., Miquel R., Moodley K., Morgan R., Mroczkowski T., Nati F., Newburgh L. B., Niemack M. D., Nishizawa A. J., Miyatake H., Ogando R. L. C., Orlowski-Scherer J., Page L. A., Palmese A., Partridge B., Paz-Chinchon F., Phakathi P., Plazas A. A., Robertson N. C., Romer A. K., Carnero Rosell A., Sanchez E., Schaan E., Schillaci A., Sehgal N., Serrano S., Shin T., Simon S. M., Smith M., Salatino M., Soares-Santos M., Spergel D. N., Staggs S. T., Storer E. R., Suchyta E., Swanson M. E. C., Tarle G., Thomas D., To C., Trac H., Ullom J. N., Vale L. R., Van Lanen J., Vavagiakis E. M., De Vicente J., Wilkinson R. D., Wollack E. J., Xu Z., and Zhan Y.
Abstract: We present a catalog of 4195 optically confirmed Sunyaev–Zel’dovich (SZ) selected galaxy clusters detected with signal-to-noise ratio >4 in 13,211 deg2 of sky surveyed by the Atacama Cosmology Telescope (ACT). Cluster candidates were selected by applying a multifrequency matched filter to 98 and 150 GHz maps constructed from ACT observations obtained from 2008 to 2018 and confirmed using deep, wide-area optical surveys. The clusters span the redshift range 0.04 < z < 1.91 (median z = 0.52). The catalog contains 222 z > 1 clusters, and a total of 868 systems are new discoveries. Assuming an SZ signal versus mass-scaling relation calibrated from X-ray observations, the sample has a 90% completeness mass limit of M500c > 3.8 × 1014 Me, evaluated at z = 0.5, for clusters detected at signal-to-noise ratio >5 in maps filtered at an angular scale of 2 4. The survey has a large overlap with deep optical weak-lensing surveys that are being used to calibrate the SZ signal mass-scaling relation, such as the Dark Energy Survey (4566 deg2), the Hyper Suprime-Cam Subaru Strategic Program (469 deg2), and the Kilo Degree Survey (825 deg2). We highlight some noteworthy objects in the sample, including potentially projected systems, clusters with strong lensing features, clusters with active central galaxies or star formation, and systems of multiple clusters that may be physically associated. The cluster catalog will be a useful resource for future cosmological analyses and studying the evolution of the intracluster medium and galaxies in massive clusters over the past 10 Gyr.
Published: 2021

12. Erratum: The Simons Observatory Large Aperture Telescope Receiver (ApJS (2021) 256: 23 DOI: 10.3847/1538-4365/ac0db7)

Author: Zhu N., Zhu, N, Bhandarkar, T, Coppi, G, Kofman, A, Orlowski-Scherer, J, Xu, Z, Adachi, S, Ade, P, Aiola, S, Austermann, J, Bazarko, A, Beall, J, Bhimani, S, Bond, J, Chesmore, G, Choi, S, Connors, J, Cothard, N, Devlin, M, Dicker, S, Dober, B, Duell, C, Duff, S, Dunner, R, Fabbian, G, Galitzki, N, Gallardo, P, Golec, J, Haridas, S, Harrington, K, Healy, E, Patty Ho, S, Huber, Z, Hubmayr, J, Iuliano, J, Johnson, B, Keating, B, Kiuchi, K, Koopman, B, Lashner, J, Lee, A, Li, Y, Limon, M, Link, M, Lucas, T, Mccarrick, H, Moore, J, Nati, F, Newburgh, L, Niemack, M, Pierpaoli, E, Randall, M, Sarmiento, K, Saunders, L, Seibert, J, Sierra, C, Sonka, R, Spisak, J, Sutariya, S, Tajima, O, Teply, G, Thornton, R, Tsan, T, Tucker, C, Ullom, J, Vavagiakis, E, Vissers, M, Walker, S, Westbrook, B, Wollack, E, Zannoni, M, Zhu N., Bhandarkar T., Coppi G., Kofman A. M., Orlowski-Scherer J. L., Xu Z., Adachi S., Ade P., Aiola S., Austermann J., Bazarko A. O., Beall J. A., Bhimani S., Bond J. R., Chesmore G. E., Choi S. K., Connors J., Cothard N. F., Devlin M., Dicker S., Dober B., Duell C. J., Duff S. M., Dunner R., Fabbian G., Galitzki N., Gallardo P. A., Golec J. E., Haridas S. K., Harrington K., Healy E., Patty Ho S. -P., Huber Z. B., Hubmayr J., Iuliano J., Johnson B. R., Keating B., Kiuchi K., Koopman B. J., Lashner J., Lee A. T., Li Y., Limon M., Link M., Lucas T. J., McCarrick H., Moore J., Nati F., Newburgh L. B., Niemack M. D., Pierpaoli E., Randall M. J., Sarmiento K. P., Saunders L. J., Seibert J., Sierra C., Sonka R., Spisak J., Sutariya S., Tajima O., Teply G. P., Thornton R. J., Tsan T., Tucker C., Ullom J., Vavagiakis E. M., Vissers M. R., Walker S., Westbrook B., Wollack E. J., Zannoni M., Zhu N., Zhu, N, Bhandarkar, T, Coppi, G, Kofman, A, Orlowski-Scherer, J, Xu, Z, Adachi, S, Ade, P, Aiola, S, Austermann, J, Bazarko, A, Beall, J, Bhimani, S, Bond, J, Chesmore, G, Choi, S, Connors, J, Cothard, N, Devlin, M, Dicker, S, Dober, B, Duell, C, Duff, S, Dunner, R, Fabbian, G, Galitzki, N, Gallardo, P, Golec, J, Haridas, S, Harrington, K, Healy, E, Patty Ho, S, Huber, Z, Hubmayr, J, Iuliano, J, Johnson, B, Keating, B, Kiuchi, K, Koopman, B, Lashner, J, Lee, A, Li, Y, Limon, M, Link, M, Lucas, T, Mccarrick, H, Moore, J, Nati, F, Newburgh, L, Niemack, M, Pierpaoli, E, Randall, M, Sarmiento, K, Saunders, L, Seibert, J, Sierra, C, Sonka, R, Spisak, J, Sutariya, S, Tajima, O, Teply, G, Thornton, R, Tsan, T, Tucker, C, Ullom, J, Vavagiakis, E, Vissers, M, Walker, S, Westbrook, B, Wollack, E, Zannoni, M, Zhu N., Bhandarkar T., Coppi G., Kofman A. M., Orlowski-Scherer J. L., Xu Z., Adachi S., Ade P., Aiola S., Austermann J., Bazarko A. O., Beall J. A., Bhimani S., Bond J. R., Chesmore G. E., Choi S. K., Connors J., Cothard N. F., Devlin M., Dicker S., Dober B., Duell C. J., Duff S. M., Dunner R., Fabbian G., Galitzki N., Gallardo P. A., Golec J. E., Haridas S. K., Harrington K., Healy E., Patty Ho S. -P., Huber Z. B., Hubmayr J., Iuliano J., Johnson B. R., Keating B., Kiuchi K., Koopman B. J., Lashner J., Lee A. T., Li Y., Limon M., Link M., Lucas T. J., McCarrick H., Moore J., Nati F., Newburgh L. B., Niemack M. D., Pierpaoli E., Randall M. J., Sarmiento K. P., Saunders L. J., Seibert J., Sierra C., Sonka R., Spisak J., Sutariya S., Tajima O., Teply G. P., Thornton R. J., Tsan T., Tucker C., Ullom J., Vavagiakis E. M., Vissers M. R., Walker S., Westbrook B., Wollack E. J., and Zannoni M.
Abstract: After the publication of the article, it was brought to our attention that the description of Equation (1) may cause potential confusion. Thus, we have decided to provide a newer reference and added a unit for qtot in the description. The updated paragraph should read as the following:.
Published: 2021

13. The mass and galaxy distribution around SZ-selected clusters

Author: Shin, T, Jain, B, Adhikari, S, Baxter, E, Chang, C, Pandey, S, Salcedo, A, Weinberg, D, Amsellem, A, Battaglia, N, Belyakov, M, Dacunha, T, Goldstein, S, Kravtsov, A, Varga, T, Abbott, T, Aguena, M, Alarcon, A, Allam, S, Amon, A, Andrade-Oliveira, F, Annis, J, Bacon, D, Bechtol, K, Becker, M, Bernstein, G, Bertin, E, Bocquet, S, Bond, J, Brooks, D, Buckley-Geer, E, Burke, D, Campos, A, Carnero Rosell, A, Carrasco Kind, M, Carretero, J, Chen, R, Choi, A, Costanzi, M, da Costa, L, Derose, J, Desai, S, de Vicente, J, Devlin, M, Diehl, H, Dietrich, J, Dodelson, S, Doel, P, Doux, C, Drlica-Wagner, A, Eckert, K, Elvin-Poole, J, Everett, S, Ferraro, S, Ferrero, I, Ferte, A, Flaugher, B, Frieman, J, Gallardo, P, Gatti, M, Gaztanaga, E, Gerdes, D, Gruen, D, Gruendl, R, Gutierrez, G, Harrison, I, Hartley, W, Hill, J, Hilton, M, Hinton, S, Hollowood, D, Hughes, J, James, D, Jarvis, M, Jeltema, T, Koopman, B, Krause, E, Kuehn, K, Kuropatkin, N, Lahav, O, Lima, M, Lokken, M, Maccrann, N, Madhavacheril, M, Maia, M, Mccullough, J, Mcmahon, J, Melchior, P, Menanteau, F, Miquel, R, Mohr, J, Moodley, K, Morgan, R, Myles, J, Nati, F, Navarro-Alsina, A, Niemack, M, Ogando, R, Page, L, Palmese, A, Partridge, B, Paz-Chinchon, F, Pereira, M, Pieres, A, Plazas Malagon, A, Prat, J, Raveri, M, Rodriguez-Monroy, M, Rollins, R, Romer, A, Rykoff, E, Salatino, M, Sanchez, C, Sanchez, E, Santiago, B, Scarpine, V, Schillaci, A, Secco, L, Serrano, S, Sevilla-Noarbe, I, Sheldon, E, Sherwin, B, Sifon, C, Smith, M, Soares-Santos, M, Staggs, S, Suchyta, E, Swanson, M, Tarle, G, Thomas, D, To, C, Troxel, M, Tutusaus, I, Vavagiakis, E, Weller, J, Wollack, E, Yanny, B, Yin, B, Zhang, Y, Shin T., Jain B., Adhikari S., Baxter E. J., Chang C., Pandey S., Salcedo A., Weinberg D. H., Amsellem A., Battaglia N., Belyakov M., Dacunha T., Goldstein S., Kravtsov A. V., Varga T. N., Abbott T. M. C., Aguena M., Alarcon A., Allam S., Amon A., Andrade-Oliveira F., Annis J., Bacon D., Bechtol K., Becker M. R., Bernstein G. M., Bertin E., Bocquet S., Bond J. R., Brooks D., Buckley-Geer E., Burke D. L., Campos A., Carnero Rosell A., Carrasco Kind M., Carretero J., Chen R., Choi A., Costanzi M., da Costa L. N., DeRose J., Desai S., de Vicente J., Devlin M. J., Diehl H. T., Dietrich J. P., Dodelson S., Doel P., Doux C., Drlica-Wagner A., Eckert K., Elvin-Poole J., Everett S., Ferraro S., Ferrero I., Ferte A., Flaugher B., Frieman J., Gallardo P. A., Gatti M., Gaztanaga E., Gerdes D. W., Gruen D., Gruendl R. A., Gutierrez G., Harrison I., Hartley W. G., Hill J. C., Hilton M., Hinton S. R., Hollowood D. L., Hughes J. P., James D. J., Jarvis M., Jeltema T., Koopman B. J., Krause E., Kuehn K., Kuropatkin N., Lahav O., Lima M., Lokken M., MacCrann N., Madhavacheril M. S., Maia M. A. G., McCullough J., McMahon J., Melchior P., Menanteau F., Miquel R., Mohr J. J., Moodley K., Morgan R., Myles J., Nati F., Navarro-Alsina A., Niemack M. D., Ogando R. L. C., Page L. A., Palmese A., Partridge B., Paz-Chinchon F., Pereira M. E. S., Pieres A., Plazas Malagon A. A., Prat J., Raveri M., Rodriguez-Monroy M., Rollins R. P., Romer A. K., Rykoff E. S., Salatino M., Sanchez C., Sanchez E., Santiago B., Scarpine V., Schillaci A., Secco L. F., Serrano S., Sevilla-Noarbe I., Sheldon E., Sherwin B. D., Sifon C., Smith M., Soares-Santos M., Staggs S. T., Suchyta E., Swanson M. E. C., Tarle G., Thomas D., To C., Troxel M. A., Tutusaus I., Vavagiakis E. M., Weller J., Wollack E. J., Yanny B., Yin B., Zhang Y., Shin, T, Jain, B, Adhikari, S, Baxter, E, Chang, C, Pandey, S, Salcedo, A, Weinberg, D, Amsellem, A, Battaglia, N, Belyakov, M, Dacunha, T, Goldstein, S, Kravtsov, A, Varga, T, Abbott, T, Aguena, M, Alarcon, A, Allam, S, Amon, A, Andrade-Oliveira, F, Annis, J, Bacon, D, Bechtol, K, Becker, M, Bernstein, G, Bertin, E, Bocquet, S, Bond, J, Brooks, D, Buckley-Geer, E, Burke, D, Campos, A, Carnero Rosell, A, Carrasco Kind, M, Carretero, J, Chen, R, Choi, A, Costanzi, M, da Costa, L, Derose, J, Desai, S, de Vicente, J, Devlin, M, Diehl, H, Dietrich, J, Dodelson, S, Doel, P, Doux, C, Drlica-Wagner, A, Eckert, K, Elvin-Poole, J, Everett, S, Ferraro, S, Ferrero, I, Ferte, A, Flaugher, B, Frieman, J, Gallardo, P, Gatti, M, Gaztanaga, E, Gerdes, D, Gruen, D, Gruendl, R, Gutierrez, G, Harrison, I, Hartley, W, Hill, J, Hilton, M, Hinton, S, Hollowood, D, Hughes, J, James, D, Jarvis, M, Jeltema, T, Koopman, B, Krause, E, Kuehn, K, Kuropatkin, N, Lahav, O, Lima, M, Lokken, M, Maccrann, N, Madhavacheril, M, Maia, M, Mccullough, J, Mcmahon, J, Melchior, P, Menanteau, F, Miquel, R, Mohr, J, Moodley, K, Morgan, R, Myles, J, Nati, F, Navarro-Alsina, A, Niemack, M, Ogando, R, Page, L, Palmese, A, Partridge, B, Paz-Chinchon, F, Pereira, M, Pieres, A, Plazas Malagon, A, Prat, J, Raveri, M, Rodriguez-Monroy, M, Rollins, R, Romer, A, Rykoff, E, Salatino, M, Sanchez, C, Sanchez, E, Santiago, B, Scarpine, V, Schillaci, A, Secco, L, Serrano, S, Sevilla-Noarbe, I, Sheldon, E, Sherwin, B, Sifon, C, Smith, M, Soares-Santos, M, Staggs, S, Suchyta, E, Swanson, M, Tarle, G, Thomas, D, To, C, Troxel, M, Tutusaus, I, Vavagiakis, E, Weller, J, Wollack, E, Yanny, B, Yin, B, Zhang, Y, Shin T., Jain B., Adhikari S., Baxter E. J., Chang C., Pandey S., Salcedo A., Weinberg D. H., Amsellem A., Battaglia N., Belyakov M., Dacunha T., Goldstein S., Kravtsov A. V., Varga T. N., Abbott T. M. C., Aguena M., Alarcon A., Allam S., Amon A., Andrade-Oliveira F., Annis J., Bacon D., Bechtol K., Becker M. R., Bernstein G. M., Bertin E., Bocquet S., Bond J. R., Brooks D., Buckley-Geer E., Burke D. L., Campos A., Carnero Rosell A., Carrasco Kind M., Carretero J., Chen R., Choi A., Costanzi M., da Costa L. N., DeRose J., Desai S., de Vicente J., Devlin M. J., Diehl H. T., Dietrich J. P., Dodelson S., Doel P., Doux C., Drlica-Wagner A., Eckert K., Elvin-Poole J., Everett S., Ferraro S., Ferrero I., Ferte A., Flaugher B., Frieman J., Gallardo P. A., Gatti M., Gaztanaga E., Gerdes D. W., Gruen D., Gruendl R. A., Gutierrez G., Harrison I., Hartley W. G., Hill J. C., Hilton M., Hinton S. R., Hollowood D. L., Hughes J. P., James D. J., Jarvis M., Jeltema T., Koopman B. J., Krause E., Kuehn K., Kuropatkin N., Lahav O., Lima M., Lokken M., MacCrann N., Madhavacheril M. S., Maia M. A. G., McCullough J., McMahon J., Melchior P., Menanteau F., Miquel R., Mohr J. J., Moodley K., Morgan R., Myles J., Nati F., Navarro-Alsina A., Niemack M. D., Ogando R. L. C., Page L. A., Palmese A., Partridge B., Paz-Chinchon F., Pereira M. E. S., Pieres A., Plazas Malagon A. A., Prat J., Raveri M., Rodriguez-Monroy M., Rollins R. P., Romer A. K., Rykoff E. S., Salatino M., Sanchez C., Sanchez E., Santiago B., Scarpine V., Schillaci A., Secco L. F., Serrano S., Sevilla-Noarbe I., Sheldon E., Sherwin B. D., Sifon C., Smith M., Soares-Santos M., Staggs S. T., Suchyta E., Swanson M. E. C., Tarle G., Thomas D., To C., Troxel M. A., Tutusaus I., Vavagiakis E. M., Weller J., Wollack E. J., Yanny B., Yin B., and Zhang Y.
Abstract: We present measurements of the radial profiles of the mass and galaxy number density around Sunyaev–Zel’dovich (SZ)-selected clusters using both weak lensing and galaxy counts. The clusters are selected from the Atacama Cosmology Telescope Data Release 5 and the galaxies from the Dark Energy Survey Year 3 data set. With signal-to-noise ratio of 62 (45) for galaxy (weak lensing) profiles over scales of about 0.2–20 h-1 Mpc, these are the highest precision measurements for SZ-selected clusters to date. Because SZ selection closely approximates mass selection, these measurements enable several tests of theoretical models of the mass and light distribution around clusters. Our main findings are: (1) The splashback feature is detected at a consistent location in both the mass and galaxy profiles and its location is consistent with predictions of cold dark matter N-body simulations. (2) The full mass profile is also consistent with the simulations. (3) The shapes of the galaxy and lensing profiles are remarkably similar for our sample over the entire range of scales, from well inside the cluster halo to the quasilinear regime. We measure the dependence of the profile shapes on the galaxy sample, redshift, and cluster mass. We extend the Diemer & Kravtsov model for the cluster profiles to the linear regime using perturbation theory and show that it provides a good match to the measured profiles. We also compare the measured profiles to predictions of the standard halo model and simulations that include hydrodynamics. Applications of these results to cluster mass estimation, cosmology, and astrophysics are discussed.
Published: 2021

14. Atacama Cosmology Telescope measurements of a large sample of candidates from the Massive and Distant Clusters of WISE Survey: Sunyaev-Zeldovich effect confirmation of MaDCoWS candidates using ACT

Author: Orlowski-Scherer, J, Di Mascolo, L, Bhandarkar, T, Manduca, A, Mroczkowski, T, Amodeo, S, Battaglia, N, Brodwin, M, Choi, S, Devlin, M, Dicker, S, Dunkley, J, Gonzalez, A, Han, D, Hilton, M, Huffenberger, K, Hughes, J, Macinnis, A, Knowles, K, Koopman, B, Lowe, I, Moodley, K, Nati, F, Niemack, M, Page, L, Partridge, B, Romero, C, Salatino, M, Schillaci, A, Sehgal, N, Sifon, C, Staggs, S, Stanford, S, Thornton, R, Vavagiakis, E, Wollack, E, Xu, Z, Zhu, N, Orlowski-Scherer J., Di Mascolo L., Bhandarkar T., Manduca A., Mroczkowski T., Amodeo S., Battaglia N., Brodwin M., Choi S. K., Devlin M., Dicker S., Dunkley J., Gonzalez A. H., Han D., Hilton M., Huffenberger K., Hughes J. P., MacInnis A., Knowles K., Koopman B. J., Lowe I., Moodley K., Nati F., Niemack M. D., Page L. A., Partridge B., Romero C., Salatino M., Schillaci A., Sehgal N., Sifon C., Staggs S., Stanford S. A., Thornton R., Vavagiakis E. M., Wollack E. J., Xu Z., Zhu N., Orlowski-Scherer, J, Di Mascolo, L, Bhandarkar, T, Manduca, A, Mroczkowski, T, Amodeo, S, Battaglia, N, Brodwin, M, Choi, S, Devlin, M, Dicker, S, Dunkley, J, Gonzalez, A, Han, D, Hilton, M, Huffenberger, K, Hughes, J, Macinnis, A, Knowles, K, Koopman, B, Lowe, I, Moodley, K, Nati, F, Niemack, M, Page, L, Partridge, B, Romero, C, Salatino, M, Schillaci, A, Sehgal, N, Sifon, C, Staggs, S, Stanford, S, Thornton, R, Vavagiakis, E, Wollack, E, Xu, Z, Zhu, N, Orlowski-Scherer J., Di Mascolo L., Bhandarkar T., Manduca A., Mroczkowski T., Amodeo S., Battaglia N., Brodwin M., Choi S. K., Devlin M., Dicker S., Dunkley J., Gonzalez A. H., Han D., Hilton M., Huffenberger K., Hughes J. P., MacInnis A., Knowles K., Koopman B. J., Lowe I., Moodley K., Nati F., Niemack M. D., Page L. A., Partridge B., Romero C., Salatino M., Schillaci A., Sehgal N., Sifon C., Staggs S., Stanford S. A., Thornton R., Vavagiakis E. M., Wollack E. J., Xu Z., and Zhu N.
Abstract: Context. Galaxy clusters are an important tool for cosmology, and their detection and characterization are key goals for current and future surveys. Using data from the Wide-field Infrared Survey Explorer (WISE), the Massive and Distant Clusters of WISE Survey (MaDCoWS) located 2839 significant galaxy overdensities at redshifts 0.7-1.5, which included extensive follow-up imaging from the Spitzer Space Telescope to determine cluster richnesses. Concurrently, the Atacama Cosmology Telescope (ACT) has produced large area millimeter-wave maps in three frequency bands along with a large catalog of Sunyaev-Zeldovich (SZ)-selected clusters as part of its Data Release 5 (DR5). Aims. We aim to verify and characterize MaDCoWS clusters using measurements of, or limits on, their thermal SZ effect signatures. We also use these detections to establish the scaling relation between SZ mass and the MaDCoWS-defined richness. Methods. Using the maps and cluster catalog from DR5, we explore the scaling between SZ mass and cluster richness. We do this by comparing cataloged detections and extracting individual and stacked SZ signals from the MaDCoWS cluster locations. We use complementary radio survey data from the Very Large Array, submillimeter data from Herschel, and ACT 224 GHz data to assess the impact of contaminating sources on the SZ signals from both ACT and MaDCoWS clusters. We use a hierarchical Bayesian model to fit the mass-richness scaling relation, allowing for clusters to be drawn from two populations: one, a Gaussian centered on the mass-richness relation, and the other, a Gaussian centered on zero SZ signal. Results. We find that MaDCoWS clusters have submillimeter contamination that is consistent with a gray-body spectrum, while the ACT clusters are consistent with no submillimeter emission on average. Additionally, the intrinsic radio intensities of ACT clusters are lower than those of MaDCoWS clusters, even when the ACT clusters are restricted to the same redshift r
Published: 2021

15. The atacama cosmology telescope: Summary of dr4 and dr5 data products and data access

Author: Mallaby-Kay, M, Atkins, Z, Aiola, S, Amodeo, S, Austermann, J, Beall, J, Becker, D, Bond, J, Calabrese, E, Chesmore, G, Choi, S, Crowley, K, Darwish, O, Denison, E, Devlin, M, Duff, S, Duivenvoorden, A, Dunkley, J, Ferraro, S, Fichman, K, Gallardo, P, Golec, J, Guan, Y, Han, D, Hasselfield, M, Hill, J, Hilton, G, Hilton, M, Hlozek, R, Hubmayr, J, Huffenberger, K, Hughes, J, Koopman, B, Louis, T, Macinnis, A, Madhavacheril, M, Mcmahon, J, Moodley, K, Naess, S, Namikawa, T, Nati, F, Newburgh, L, Nibarger, J, Niemack, M, Page, L, Salatino, M, Schaan, E, Schillaci, A, Sehgal, N, Sherwin, B, Sifon, C, Simon, S, Staggs, S, Storer, E, Ullom, J, Van Engelen, A, Van Lanen, J, Vale, L, Wollack, E, Xu, Z, Mallaby-Kay M., Atkins Z., Aiola S., Amodeo S., Austermann J. E., Beall J. A., Becker D. T., Bond J. R., Calabrese E., Chesmore G. E., Choi S. K., Crowley K. T., Darwish O., Denison E. V., Devlin M. J., Duff S. M., Duivenvoorden A. J., Dunkley J., Ferraro S., Fichman K., Gallardo P. A., Golec J. E., Guan Y., Han D., Hasselfield M., Hill J. C., Hilton G. C., Hilton M., Hlozek R., Hubmayr J., Huffenberger K. M., Hughes J. P., Koopman B. J., Louis T., MacInnis A., Madhavacheril M. S., McMahon J., Moodley K., Naess S., Namikawa T., Nati F., Newburgh L. B., Nibarger J. P., Niemack M. D., Page L. A., Salatino M., Schaan E., Schillaci A., Sehgal N., Sherwin B. D., Sifon C., Simon S., Staggs S. T., Storer E. R., Ullom J. N., Van Engelen A., Van Lanen J., Vale L. R., Wollack E. J., Xu Z., Mallaby-Kay, M, Atkins, Z, Aiola, S, Amodeo, S, Austermann, J, Beall, J, Becker, D, Bond, J, Calabrese, E, Chesmore, G, Choi, S, Crowley, K, Darwish, O, Denison, E, Devlin, M, Duff, S, Duivenvoorden, A, Dunkley, J, Ferraro, S, Fichman, K, Gallardo, P, Golec, J, Guan, Y, Han, D, Hasselfield, M, Hill, J, Hilton, G, Hilton, M, Hlozek, R, Hubmayr, J, Huffenberger, K, Hughes, J, Koopman, B, Louis, T, Macinnis, A, Madhavacheril, M, Mcmahon, J, Moodley, K, Naess, S, Namikawa, T, Nati, F, Newburgh, L, Nibarger, J, Niemack, M, Page, L, Salatino, M, Schaan, E, Schillaci, A, Sehgal, N, Sherwin, B, Sifon, C, Simon, S, Staggs, S, Storer, E, Ullom, J, Van Engelen, A, Van Lanen, J, Vale, L, Wollack, E, Xu, Z, Mallaby-Kay M., Atkins Z., Aiola S., Amodeo S., Austermann J. E., Beall J. A., Becker D. T., Bond J. R., Calabrese E., Chesmore G. E., Choi S. K., Crowley K. T., Darwish O., Denison E. V., Devlin M. J., Duff S. M., Duivenvoorden A. J., Dunkley J., Ferraro S., Fichman K., Gallardo P. A., Golec J. E., Guan Y., Han D., Hasselfield M., Hill J. C., Hilton G. C., Hilton M., Hlozek R., Hubmayr J., Huffenberger K. M., Hughes J. P., Koopman B. J., Louis T., MacInnis A., Madhavacheril M. S., McMahon J., Moodley K., Naess S., Namikawa T., Nati F., Newburgh L. B., Nibarger J. P., Niemack M. D., Page L. A., Salatino M., Schaan E., Schillaci A., Sehgal N., Sherwin B. D., Sifon C., Simon S., Staggs S. T., Storer E. R., Ullom J. N., Van Engelen A., Van Lanen J., Vale L. R., Wollack E. J., and Xu Z.
Abstract: Two recent large data releases for the Atacama Cosmology Telescope (ACT), called DR4 and DR5, are available for public access. These data include temperature and polarization maps that cover nearly half the sky at arcminute resolution in three frequency bands; lensing maps and component-separated maps covering ~2100 deg2 of sky; derived power spectra and cosmological likelihoods; a catalog of over 4000 galaxy clusters; and supporting ancillary products including beam functions and masks. The data and products are described in a suite of ACT papers; here we provide a summary. In order to facilitate ease of access to these data, we present a set of Jupyter IPython notebooks developed to introduce users to DR4, DR5, and the tools needed to analyze these data. The data products (excluding simulations) and the set of notebooks are publicly available on the NASA Legacy Archive for Microwave Background Data Analysis; simulation products are available on the National Energy Research Scientific Computing Center.
Published: 2021

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

Author: Vavagiakis, E, Gallardo, P, Calafut, V, Amodeo, S, Aiola, S, Austermann, J, Battaglia, N, Battistelli, E, Beall, J, Bean, R, Bond, J, Calabrese, E, Choi, S, Cothard, N, Devlin, M, Duell, C, Duff, S, Duivenvoorden, A, Dunkley, J, Dunner, R, Ferraro, S, Guan, Y, Hill, J, Hilton, G, Hilton, M, Hlozek, R, Huber, Z, Hubmayr, J, Huffenberger, K, Hughes, J, Koopman, B, Kosowsky, A, Li, Y, Lokken, M, Madhavacheril, M, Mcmahon, J, Moodley, K, Naess, S, Nati, F, Newburgh, L, Niemack, M, Page, L, Partridge, B, Schaan, E, Schillaci, A, Sifon, C, Spergel, D, Staggs, S, Ullom, J, Vale, L, Van Engelen, A, Van Lanen, J, Wollack, E, Xu, Z, Vavagiakis E. M., Gallardo P. A., Calafut V., Amodeo S., Aiola S., Austermann J. E., Battaglia N., Battistelli E. S., Beall J. A., Bean R., Bond J. R., Calabrese E., Choi S. K., Cothard N. F., Devlin M. J., Duell C. J., Duff S. M., Duivenvoorden A. J., Dunkley J., Dunner R., Ferraro S., Guan Y., Hill J. C., Hilton G. C., Hilton M., Hlozek R., Huber Z. B., Hubmayr J., Huffenberger K. M., Hughes J. P., Koopman B. J., Kosowsky A., Li Y., Lokken M., Madhavacheril M., McMahon J., Moodley K., Naess S., Nati F., Newburgh L. B., Niemack M. D., Page L. A., Partridge B., Schaan E., Schillaci A., Sifon C., Spergel D. N., Staggs S. T., Ullom J. N., Vale L. R., Van Engelen A., Van Lanen J., Wollack E. J., Xu Z., Vavagiakis, E, Gallardo, P, Calafut, V, Amodeo, S, Aiola, S, Austermann, J, Battaglia, N, Battistelli, E, Beall, J, Bean, R, Bond, J, Calabrese, E, Choi, S, Cothard, N, Devlin, M, Duell, C, Duff, S, Duivenvoorden, A, Dunkley, J, Dunner, R, Ferraro, S, Guan, Y, Hill, J, Hilton, G, Hilton, M, Hlozek, R, Huber, Z, Hubmayr, J, Huffenberger, K, Hughes, J, Koopman, B, Kosowsky, A, Li, Y, Lokken, M, Madhavacheril, M, Mcmahon, J, Moodley, K, Naess, S, Nati, F, Newburgh, L, Niemack, M, Page, L, Partridge, B, Schaan, E, Schillaci, A, Sifon, C, Spergel, D, Staggs, S, Ullom, J, Vale, L, Van Engelen, A, Van Lanen, J, Wollack, E, Xu, Z, Vavagiakis E. M., Gallardo P. A., Calafut V., Amodeo S., Aiola S., Austermann J. E., Battaglia N., Battistelli E. S., Beall J. A., Bean R., Bond J. R., Calabrese E., Choi S. K., Cothard N. F., Devlin M. J., Duell C. J., Duff S. M., Duivenvoorden A. J., Dunkley J., Dunner R., Ferraro S., Guan Y., Hill J. C., Hilton G. C., Hilton M., Hlozek R., Huber Z. B., Hubmayr J., Huffenberger K. M., Hughes J. P., Koopman B. J., Kosowsky A., Li Y., Lokken M., Madhavacheril M., McMahon J., Moodley K., Naess S., Nati F., Newburgh L. B., Niemack M. D., Page L. A., Partridge B., Schaan E., Schillaci A., Sifon C., Spergel D. N., Staggs S. T., Ullom J. N., Vale L. R., Van Engelen A., Van Lanen J., Wollack E. J., and Xu Z.
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

17. The Atacama Cosmology Telescope: Microwave Intensity and Polarization Maps of the Galactic Center

Author: Guan, Y, Clark, S, Hensley, B, Gallardo, P, Naess, S, Duell, C, Aiola, S, Atkins, Z, Calabrese, E, Choi, S, Cothard, N, Devlin, M, Duivenvoorden, A, Dunkley, J, Dunner, R, Ferraro, S, Hasselfield, M, Hughes, J, Koopman, B, Kosowsky, A, Madhavacheril, M, Mcmahon, J, Nati, F, Niemack, M, Page, L, Salatino, M, Schaan, E, Sehgal, N, Sifon, C, Staggs, S, Vavagiakis, E, Wollack, E, Xu, Z, Guan Y., Clark S. E., Hensley B. S., Gallardo P. A., Naess S., Duell C. J., Aiola S., Atkins Z., Calabrese E., Choi S. K., Cothard N. F., Devlin M., Duivenvoorden A. J., Dunkley J., Dunner R., Ferraro S., Hasselfield M., Hughes J. P., Koopman B. J., Kosowsky A. B., Madhavacheril M. S., McMahon J., Nati F., Niemack M. D., Page L. A., Salatino M., Schaan E., Sehgal N., Sifon C., Staggs S., Vavagiakis E. M., Wollack E. J., Xu Z., Guan, Y, Clark, S, Hensley, B, Gallardo, P, Naess, S, Duell, C, Aiola, S, Atkins, Z, Calabrese, E, Choi, S, Cothard, N, Devlin, M, Duivenvoorden, A, Dunkley, J, Dunner, R, Ferraro, S, Hasselfield, M, Hughes, J, Koopman, B, Kosowsky, A, Madhavacheril, M, Mcmahon, J, Nati, F, Niemack, M, Page, L, Salatino, M, Schaan, E, Sehgal, N, Sifon, C, Staggs, S, Vavagiakis, E, Wollack, E, Xu, Z, Guan Y., Clark S. E., Hensley B. S., Gallardo P. A., Naess S., Duell C. J., Aiola S., Atkins Z., Calabrese E., Choi S. K., Cothard N. F., Devlin M., Duivenvoorden A. J., Dunkley J., Dunner R., Ferraro S., Hasselfield M., Hughes J. P., Koopman B. J., Kosowsky A. B., Madhavacheril M. S., McMahon J., Nati F., Niemack M. D., Page L. A., Salatino M., Schaan E., Sehgal N., Sifon C., Staggs S., Vavagiakis E. M., Wollack E. J., and Xu Z.
Abstract: We present arcminute-resolution intensity and polarization maps of the Galactic center made with the Atacama Cosmology Telescope. The maps cover a 32 deg2 field at 98, 150, and 224 GHz with |l| ≤ 4 , |b| ≤ 2 . We combine these data with Planck observations at similar frequencies to create coadded maps with increased sensitivity at large angular scales. With the coadded maps, we are able to resolve many known features of the Central Molecular Zone (CMZ) in both total intensity and polarization. We map the orientation of the plane-of-sky component of the Galactic magnetic field inferred from the polarization angle in the CMZ, finding significant changes in morphology in the three frequency bands as the underlying dominant emission mechanism changes from synchrotron to dust emission. Selected Galactic center sources, including Sgr A∗, the Brick molecular cloud (G0.253+0.016), the Mouse pulsar wind nebula (G359.23-0.82), and the Tornado supernova remnant candidate (G357.7-0.1), are examined in detail. These data illustrate the potential for leveraging ground-based cosmic microwave background polarization experiments for Galactic science.
Published: 2021

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

Author: Calafut, V, Gallardo, P, Vavagiakis, E, Amodeo, S, Aiola, S, Austermann, J, Battaglia, N, Battistelli, E, Beall, J, Bean, R, Bond, J, Calabrese, E, Choi, S, Cothard, N, Devlin, M, Duell, C, Duff, S, Duivenvoorden, A, Dunkley, J, Dunner, R, Ferraro, S, Guan, Y, Hill, J, Hilton, G, Hilton, M, Hlozek, R, Huber, Z, Hubmayr, J, Huffenberger, K, Hughes, J, Koopman, B, Kosowsky, A, Li, Y, Lokken, M, Madhavacheril, M, Mcmahon, J, Moodley, K, Naess, S, Nati, F, Newburgh, L, Niemack, M, Page, L, Partridge, B, Schaan, E, Schillaci, A, Sifon, C, Spergel, D, Staggs, S, Ullom, J, Vale, L, Van Engelen, A, Van Lanen, J, Wollack, E, Xu, Z, Calafut V., Gallardo P. A., Vavagiakis E. M., Amodeo S., Aiola S., Austermann J. E., Battaglia N., Battistelli E. S., Beall J. A., Bean R., Bond J. R., Calabrese E., Choi S. K., Cothard N. F., Devlin M. J., Duell C. J., Duff S. M., Duivenvoorden A. J., Dunkley J., Dunner R., Ferraro S., Guan Y., Hill J. C., Hilton G. C., Hilton M., Hlozek R., Huber Z. B., Hubmayr J., Huffenberger K. M., Hughes J. P., Koopman B. J., Kosowsky A., Li Y., Lokken M., Madhavacheril M., McMahon J., Moodley K., Naess S., Nati F., Newburgh L. B., Niemack M. D., Page L. A., Partridge B., Schaan E., Schillaci A., Sifon C., Spergel D. N., Staggs S. T., Ullom J. N., Vale L. R., Van Engelen A., Van Lanen J., Wollack E. J., Xu Z., Calafut, V, Gallardo, P, Vavagiakis, E, Amodeo, S, Aiola, S, Austermann, J, Battaglia, N, Battistelli, E, Beall, J, Bean, R, Bond, J, Calabrese, E, Choi, S, Cothard, N, Devlin, M, Duell, C, Duff, S, Duivenvoorden, A, Dunkley, J, Dunner, R, Ferraro, S, Guan, Y, Hill, J, Hilton, G, Hilton, M, Hlozek, R, Huber, Z, Hubmayr, J, Huffenberger, K, Hughes, J, Koopman, B, Kosowsky, A, Li, Y, Lokken, M, Madhavacheril, M, Mcmahon, J, Moodley, K, Naess, S, Nati, F, Newburgh, L, Niemack, M, Page, L, Partridge, B, Schaan, E, Schillaci, A, Sifon, C, Spergel, D, Staggs, S, Ullom, J, Vale, L, Van Engelen, A, Van Lanen, J, Wollack, E, Xu, Z, Calafut V., Gallardo P. A., Vavagiakis E. M., Amodeo S., Aiola S., Austermann J. E., Battaglia N., Battistelli E. S., Beall J. A., Bean R., Bond J. R., Calabrese E., Choi S. K., Cothard N. F., Devlin M. J., Duell C. J., Duff S. M., Duivenvoorden A. J., Dunkley J., Dunner R., Ferraro S., Guan Y., Hill J. C., Hilton G. C., Hilton M., Hlozek R., Huber Z. B., Hubmayr J., Huffenberger K. M., Hughes J. P., Koopman B. J., Kosowsky A., Li Y., Lokken M., Madhavacheril M., McMahon J., Moodley K., Naess S., Nati F., Newburgh L. B., Niemack M. D., Page L. A., Partridge B., Schaan E., Schillaci A., Sifon C., Spergel D. N., Staggs S. T., Ullom J. N., Vale L. R., Van Engelen A., Van Lanen J., Wollack E. J., and Xu Z.
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

19. Probing Galaxy Evolution in Massive Clusters Using ACT and DES: Splashback as a Cosmic Clock

Author: Adhikari, S, Shin, T, Jain, B, Hilton, M, Baxter, E, Chang, C, Wechsler, R, Battaglia, N, Bond, J, Bocquet, S, Choi, S, Derose, J, Devlin, M, Dunkley, J, Evrard, A, Ferraro, S, Hill, J, Hughes, J, Gallardo, P, Lokken, M, Macinnis, A, Madhavacheril, M, Mcmahon, J, Nati, F, Newburgh, L, Niemack, M, Page, L, Palmese, A, Partridge, B, Rozo, E, Rykoff, E, Salatino, M, Schillaci, A, Sehgal, N, Sifon, C, To, C, Wollack, E, Wu, H, Xu, Z, Aguena, M, Allam, S, Amon, A, Annis, J, Avila, S, Bacon, D, Bertin, E, Bhargava, S, Brooks, D, Burke, D, Rosell, A, Kind, M, Carretero, J, Castander, F, Choi, A, Costanzi, M, Da Costa, L, Vicente, J, Desai, S, Diehl, T, Doel, P, Everett, S, Ferrero, I, Ferte, A, Flaugher, B, Fosalba, P, Frieman, J, Garcia-Bellido, J, Gaztanaga, E, Gruen, D, Gruendl, R, Gschwend, J, Gutierrez, G, Hartley, W, Hinton, S, Hollowood, D, Honscheid, K, James, D, Jeltema, T, Kuehn, K, Kuropatkin, N, Lahav, O, Lima, M, Maia, M, Marshall, J, Martini, P, Melchior, P, Menanteau, F, Miquel, R, Morgan, R, L. C. Ogando, R, Paz-Chinchon, F, Malagon, A, Sanchez, E, Santiago, B, Scarpine, V, Serrano, S, Sevilla-Noarbe, I, Smith, M, Soares-Santos, M, Suchyta, E, E. C. Swanson, M, Varga, T, Wilkinson, R, Zhang, Y, Austermann, J, Beall, J, Becker, D, Denison, E, Duff, S, Hilton, G, Hubmayr, J, Ullom, J, Lanen, J, Vale, L, Adhikari S., Shin T. -H., Jain B., Hilton M., Baxter E., Chang C., Wechsler R. H., Battaglia N., Bond J. R., Bocquet S., Choi S. K., Derose J., Devlin M., Dunkley J., Evrard A. E., Ferraro S., Hill J. C., Hughes J. P., Gallardo P. A., Lokken M., Macinnis A., Madhavacheril M. S., McMahon J., Nati F., Newburgh L. B., Niemack M. D., Page L. A., Palmese A., Partridge B., Rozo E., Rykoff E., Salatino M., Schillaci A., Sehgal N., Sifon C., To C. -H., Wollack E., Wu H. -Y., Xu Z., Aguena M., Allam S., Amon A., Annis J., Avila S., Bacon D., Bertin E., Bhargava S., Brooks D., Burke D. L., Rosell A. C., Kind M. C., Carretero J., Castander F. J., Choi A., Costanzi M., Da Costa L. N., Vicente J. D., Desai S., Diehl T. H., Doel P., Everett S., Ferrero I., Ferte A., Flaugher B., Fosalba P., Frieman J., Garcia-Bellido J., Gaztanaga E., Gruen D., Gruendl R. A., Gschwend J., Gutierrez G., Hartley W. G., Hinton S. R., Hollowood D. L., Honscheid K., James D. J., Jeltema T., Kuehn K., Kuropatkin N., Lahav O., Lima M., Maia M. A. G., Marshall J. L., Martini P., Melchior P., Menanteau F., Miquel R., Morgan R., L. C. Ogando R., Paz-Chinchon F., Malagon A. P., Sanchez E., Santiago B., Scarpine V., Serrano S., Sevilla-Noarbe I., Smith M., Soares-Santos M., Suchyta E., E. C. Swanson M., Varga T. N., Wilkinson R. D., Zhang Y., Austermann J. E., Beall J. A., Becker D. T., Denison E. V., Duff S. M., Hilton G. C., Hubmayr J., Ullom J. N., Lanen J. V., Vale L. R., Adhikari, S, Shin, T, Jain, B, Hilton, M, Baxter, E, Chang, C, Wechsler, R, Battaglia, N, Bond, J, Bocquet, S, Choi, S, Derose, J, Devlin, M, Dunkley, J, Evrard, A, Ferraro, S, Hill, J, Hughes, J, Gallardo, P, Lokken, M, Macinnis, A, Madhavacheril, M, Mcmahon, J, Nati, F, Newburgh, L, Niemack, M, Page, L, Palmese, A, Partridge, B, Rozo, E, Rykoff, E, Salatino, M, Schillaci, A, Sehgal, N, Sifon, C, To, C, Wollack, E, Wu, H, Xu, Z, Aguena, M, Allam, S, Amon, A, Annis, J, Avila, S, Bacon, D, Bertin, E, Bhargava, S, Brooks, D, Burke, D, Rosell, A, Kind, M, Carretero, J, Castander, F, Choi, A, Costanzi, M, Da Costa, L, Vicente, J, Desai, S, Diehl, T, Doel, P, Everett, S, Ferrero, I, Ferte, A, Flaugher, B, Fosalba, P, Frieman, J, Garcia-Bellido, J, Gaztanaga, E, Gruen, D, Gruendl, R, Gschwend, J, Gutierrez, G, Hartley, W, Hinton, S, Hollowood, D, Honscheid, K, James, D, Jeltema, T, Kuehn, K, Kuropatkin, N, Lahav, O, Lima, M, Maia, M, Marshall, J, Martini, P, Melchior, P, Menanteau, F, Miquel, R, Morgan, R, L. C. Ogando, R, Paz-Chinchon, F, Malagon, A, Sanchez, E, Santiago, B, Scarpine, V, Serrano, S, Sevilla-Noarbe, I, Smith, M, Soares-Santos, M, Suchyta, E, E. C. Swanson, M, Varga, T, Wilkinson, R, Zhang, Y, Austermann, J, Beall, J, Becker, D, Denison, E, Duff, S, Hilton, G, Hubmayr, J, Ullom, J, Lanen, J, Vale, L, Adhikari S., Shin T. -H., Jain B., Hilton M., Baxter E., Chang C., Wechsler R. H., Battaglia N., Bond J. R., Bocquet S., Choi S. K., Derose J., Devlin M., Dunkley J., Evrard A. E., Ferraro S., Hill J. C., Hughes J. P., Gallardo P. A., Lokken M., Macinnis A., Madhavacheril M. S., McMahon J., Nati F., Newburgh L. B., Niemack M. D., Page L. A., Palmese A., Partridge B., Rozo E., Rykoff E., Salatino M., Schillaci A., Sehgal N., Sifon C., To C. -H., Wollack E., Wu H. -Y., Xu Z., Aguena M., Allam S., Amon A., Annis J., Avila S., Bacon D., Bertin E., Bhargava S., Brooks D., Burke D. L., Rosell A. C., Kind M. C., Carretero J., Castander F. J., Choi A., Costanzi M., Da Costa L. N., Vicente J. D., Desai S., Diehl T. H., Doel P., Everett S., Ferrero I., Ferte A., Flaugher B., Fosalba P., Frieman J., Garcia-Bellido J., Gaztanaga E., Gruen D., Gruendl R. A., Gschwend J., Gutierrez G., Hartley W. G., Hinton S. R., Hollowood D. L., Honscheid K., James D. J., Jeltema T., Kuehn K., Kuropatkin N., Lahav O., Lima M., Maia M. A. G., Marshall J. L., Martini P., Melchior P., Menanteau F., Miquel R., Morgan R., L. C. Ogando R., Paz-Chinchon F., Malagon A. P., Sanchez E., Santiago B., Scarpine V., Serrano S., Sevilla-Noarbe I., Smith M., Soares-Santos M., Suchyta E., E. C. Swanson M., Varga T. N., Wilkinson R. D., Zhang Y., Austermann J. E., Beall J. A., Becker D. T., Denison E. V., Duff S. M., Hilton G. C., Hubmayr J., Ullom J. N., Lanen J. V., and Vale L. R.
Abstract: We measure the projected number density profiles of galaxies and the splashback feature in clusters selected by the Sunyaev-Zel'dovich effect from the Advanced Atacama Cosmology Telescope (AdvACT) survey using galaxies observed by the Dark Energy Survey (DES). The splashback radius is consistent with CDM-only simulations and is located at 2.4-0.4+0.3 Mpc h-1. We split the galaxies on color and find significant differences in their profile shapes. Red and green-valley galaxies show a splashback-like minimum in their slope profile consistent with theory, while the bluest galaxies show a weak feature at a smaller radius. We develop a mapping of galaxies to subhalos in simulations and assign colors based on infall time onto their hosts. We find that the shift in location of the steepest slope and different profile shapes can be mapped to the average time of infall of galaxies of different colors. The steepest slope traces a discontinuity in the phase space of dark matter halos. By relating spatial profiles to infall time, we can use splashback as a clock to understand galaxy quenching. We find that red galaxies have on average been in clusters over 3.2 Gyr, green galaxies about 2.2 Gyr, while blue galaxies have been accreted most recently and have not reached apocenter. Using the full radial profiles, we fit a simple quenching model and find that the onset of galaxy quenching occurs after a delay of about a gigayear and that galaxies quench rapidly thereafter with an exponential timescale of 0.6 Gyr.
Published: 2021

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

Author: Madhavacheril, M, Hill, J, Naess, S, Addison, G, Aiola, S, Baildon, T, Battaglia, N, Bean, R, Bond, J, Calabrese, E, Calafut, V, Choi, S, Darwish, O, Datta, R, Devlin, M, Dunkley, J, Dunner, R, Ferraro, S, Gallardo, P, Gluscevic, V, Halpern, M, Han, D, Hasselfield, M, Hilton, M, Hincks, A, Hlozek, R, Ho, S, Huffenberger, K, Hughes, J, Koopman, B, Kosowsky, A, Lokken, M, Louis, T, Lungu, M, Macinnis, A, Maurin, L, Mcmahon, J, Moodley, K, Nati, F, Niemack, M, Page, L, Partridge, B, Robertson, N, Sehgal, N, Schaan, E, Schillaci, A, Sherwin, B, Sifon, C, Simon, S, Spergel, D, Staggs, S, Storer, E, Van Engelen, A, Vavagiakis, E, Wollack, E, Xu, Z, Madhavacheril M. S., Hill J. C., Naess S., Addison G. E., Aiola S., Baildon T., Battaglia N., Bean R., Bond J. R., Calabrese E., Calafut V., Choi S. K., Darwish O., Datta R., Devlin M. J., Dunkley J., Dunner R., Ferraro S., Gallardo P. A., Gluscevic V., Halpern M., Han D., Hasselfield M., Hilton M., Hincks A. D., HloZek R., Ho S. -P. P., Huffenberger K. M., Hughes J. P., Koopman B. J., Kosowsky A., Lokken M., Louis T., Lungu M., Macinnis A., Maurin L., McMahon J. J., Moodley K., Nati F., Niemack M. D., Page L. A., Partridge B., Robertson N., Sehgal N., Schaan E., Schillaci A., Sherwin B. D., Sifon C., Simon S. M., Spergel D. N., Staggs S. T., Storer E. R., Van Engelen A., Vavagiakis E. M., Wollack E. J., Xu Z., Madhavacheril, M, Hill, J, Naess, S, Addison, G, Aiola, S, Baildon, T, Battaglia, N, Bean, R, Bond, J, Calabrese, E, Calafut, V, Choi, S, Darwish, O, Datta, R, Devlin, M, Dunkley, J, Dunner, R, Ferraro, S, Gallardo, P, Gluscevic, V, Halpern, M, Han, D, Hasselfield, M, Hilton, M, Hincks, A, Hlozek, R, Ho, S, Huffenberger, K, Hughes, J, Koopman, B, Kosowsky, A, Lokken, M, Louis, T, Lungu, M, Macinnis, A, Maurin, L, Mcmahon, J, Moodley, K, Nati, F, Niemack, M, Page, L, Partridge, B, Robertson, N, Sehgal, N, Schaan, E, Schillaci, A, Sherwin, B, Sifon, C, Simon, S, Spergel, D, Staggs, S, Storer, E, Van Engelen, A, Vavagiakis, E, Wollack, E, Xu, Z, Madhavacheril M. S., Hill J. C., Naess S., Addison G. E., Aiola S., Baildon T., Battaglia N., Bean R., Bond J. R., Calabrese E., Calafut V., Choi S. K., Darwish O., Datta R., Devlin M. J., Dunkley J., Dunner R., Ferraro S., Gallardo P. A., Gluscevic V., Halpern M., Han D., Hasselfield M., Hilton M., Hincks A. D., HloZek R., Ho S. -P. P., Huffenberger K. M., Hughes J. P., Koopman B. J., Kosowsky A., Lokken M., Louis T., Lungu M., Macinnis A., Maurin L., McMahon J. J., Moodley K., Nati F., Niemack M. D., Page L. A., Partridge B., Robertson N., Sehgal N., Schaan E., Schillaci A., Sherwin B. D., Sifon C., Simon S. M., Spergel D. N., Staggs S. T., Storer E. R., Van Engelen A., Vavagiakis E. M., Wollack E. J., and Xu Z.
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

21. In-flight performance of the BLAST-TNG Kinetic Inductance Detector arrays and Readout Electronics

Author: Sinclair, A, Gordon, S, Ade, P, Ashton, P, Cho, H, Coppi, G, Corso, A, Devlin, M, Dicker, S, Dober, B, Fissel, L, Galitzky, N, Gao, J, Groppi, C, Hilton, G, Hubmayr, J, Irwin, K, Klein, J, Li, D, Lourie, N, Lowe, I, Mani, H, Mauskopf, P, Mckenney, C, Nati, F, Novak, G, Pascale, E, Pisano, G, Soler, J, Tucker, C, Underhil, M, Vissers, M, Wheeler, C, Williams, P, Sinclair A., Gordon S. B., Ade P., Ashton P., Cho H. -M., Coppi G., Corso A., Devlin M., Dicker S., Dober B., Fissel L., Galitzky N., Gao J., Groppi C., Hilton G. C., Hubmayr J., Irwin K., Klein J., Li D., Lourie N., Lowe I., Mani H., Mauskopf P. D., McKenney C., Nati F., Novak G., Pascale E., Pisano G., Soler J., Tucker C., Underhil M., Vissers M., Wheeler C., Williams P., Sinclair, A, Gordon, S, Ade, P, Ashton, P, Cho, H, Coppi, G, Corso, A, Devlin, M, Dicker, S, Dober, B, Fissel, L, Galitzky, N, Gao, J, Groppi, C, Hilton, G, Hubmayr, J, Irwin, K, Klein, J, Li, D, Lourie, N, Lowe, I, Mani, H, Mauskopf, P, Mckenney, C, Nati, F, Novak, G, Pascale, E, Pisano, G, Soler, J, Tucker, C, Underhil, M, Vissers, M, Wheeler, C, Williams, P, Sinclair A., Gordon S. B., Ade P., Ashton P., Cho H. -M., Coppi G., Corso A., Devlin M., Dicker S., Dober B., Fissel L., Galitzky N., Gao J., Groppi C., Hilton G. C., Hubmayr J., Irwin K., Klein J., Li D., Lourie N., Lowe I., Mani H., Mauskopf P. D., McKenney C., Nati F., Novak G., Pascale E., Pisano G., Soler J., Tucker C., Underhil M., Vissers M., Wheeler C., and Williams P.
Published: 2020

22. The Atacama Cosmology Telescope: Weighing Distant Clusters with the Most Ancient Light

Author: Madhavacheril, M, Sifon, C, Battaglia, N, Aiola, S, Amodeo, S, Austermann, J, Beall, J, Becker, D, Richard Bond, J, Calabrese, E, Choi, S, Denison, E, Devlin, M, Dicker, S, Duff, S, Duivenvoorden, A, Dunkley, J, Dunner, R, Ferraro, S, Gallardo, P, Guan, Y, Han, D, Colin Hill, J, Hilton, G, Hilton, M, Hubmayr, J, Huffenberger, K, Hughes, J, Koopman, B, Kosowsky, A, van Lanen, J, Lee, E, Louis, T, Macinnis, A, Mcmahon, J, Moodley, K, Naess, S, Namikawa, T, Nati, F, Newburgh, L, Niemack, M, Page, L, Partridge, B, Qu, F, Robertson, N, Salatino, M, Schaan, E, Schillaci, A, Schmitt, B, Sehgal, N, Sherwin, B, Simon, S, Spergel, D, Staggs, S, Storer, E, Ullom, J, Vale, L, van Engelen, A, Vavagiakis, E, Wollack, E, Xu, Z, Madhavacheril M. S., Sifon C., Battaglia N., Aiola S., Amodeo S., Austermann J. E., Beall J. A., Becker D. T., Richard Bond J., Calabrese E., Choi S. K., Denison E. V., Devlin M. J., Dicker S. R., Duff S. M., Duivenvoorden A. J., Dunkley J., Dunner R., Ferraro S., Gallardo P. A., Guan Y., Han D., Colin Hill J., Hilton G. C., Hilton M., Hubmayr J., Huffenberger K. M., Hughes J. P., Koopman B. J., Kosowsky A., van Lanen J., Lee E., Louis T., MacInnis A., McMahon J., Moodley K., Naess S., Namikawa T., Nati F., Newburgh L., Niemack M. D., Page L. A., Partridge B., Qu F. J., Robertson N. C., Salatino M., Schaan E., Schillaci A., Schmitt B. L., Sehgal N., Sherwin B. D., Simon S. M., Spergel D. N., Staggs S., Storer E. R., Ullom J. N., Vale L. R., van Engelen A., Vavagiakis E. M., Wollack E. J., Xu Z., Madhavacheril, M, Sifon, C, Battaglia, N, Aiola, S, Amodeo, S, Austermann, J, Beall, J, Becker, D, Richard Bond, J, Calabrese, E, Choi, S, Denison, E, Devlin, M, Dicker, S, Duff, S, Duivenvoorden, A, Dunkley, J, Dunner, R, Ferraro, S, Gallardo, P, Guan, Y, Han, D, Colin Hill, J, Hilton, G, Hilton, M, Hubmayr, J, Huffenberger, K, Hughes, J, Koopman, B, Kosowsky, A, van Lanen, J, Lee, E, Louis, T, Macinnis, A, Mcmahon, J, Moodley, K, Naess, S, Namikawa, T, Nati, F, Newburgh, L, Niemack, M, Page, L, Partridge, B, Qu, F, Robertson, N, Salatino, M, Schaan, E, Schillaci, A, Schmitt, B, Sehgal, N, Sherwin, B, Simon, S, Spergel, D, Staggs, S, Storer, E, Ullom, J, Vale, L, van Engelen, A, Vavagiakis, E, Wollack, E, Xu, Z, Madhavacheril M. S., Sifon C., Battaglia N., Aiola S., Amodeo S., Austermann J. E., Beall J. A., Becker D. T., Richard Bond J., Calabrese E., Choi S. K., Denison E. V., Devlin M. J., Dicker S. R., Duff S. M., Duivenvoorden A. J., Dunkley J., Dunner R., Ferraro S., Gallardo P. A., Guan Y., Han D., Colin Hill J., Hilton G. C., Hilton M., Hubmayr J., Huffenberger K. M., Hughes J. P., Koopman B. J., Kosowsky A., van Lanen J., Lee E., Louis T., MacInnis A., McMahon J., Moodley K., Naess S., Namikawa T., Nati F., Newburgh L., Niemack M. D., Page L. A., Partridge B., Qu F. J., Robertson N. C., Salatino M., Schaan E., Schillaci A., Schmitt B. L., Sehgal N., Sherwin B. D., Simon S. M., Spergel D. N., Staggs S., Storer E. R., Ullom J. N., Vale L. R., van Engelen A., Vavagiakis E. M., Wollack E. J., and Xu Z.
Abstract: We use gravitational lensing of the cosmic microwave background (CMB) to measure the mass of the most distant blindly selected sample of galaxy clusters on which a lensing measurement has been performed to date. In CMB data from the the Atacama Cosmology Telescope and the Planck satellite, we detect the stacked lensing effect from 677 near-infrared-selected galaxy clusters from the Massive and Distant Clusters of WISE Survey (MaDCoWS), which have a mean redshift of zñ = 1.08. There are currently no representative optical weak lensing measurements of clusters that match the distance and average mass of this sample. We detect the lensing signal with a significance of 4.2s. We model the signal with a halo model framework to find the mean mass of the population from which these clusters are drawn. Assuming that the clusters follow Navarro–Frenk–White (NFW) density profiles, we infer a mean mass of M500cñ = (1.7 + 0.4) ́ 1014 M*. We consider systematic uncertainties from cluster redshift errors, centering errors, and the shape of the NFW profile. These are all smaller than 30% of our reported uncertainty. This work highlights the potential of CMB lensing to enable cosmological constraints from the abundance of distant clusters populating ever larger volumes of the observable universe, beyond the capabilities of optical weak lensing measurements.
Published: 2020

23. Characterization, deployment, and in-flight performance of the BLAST-TNG cryogenic receiver

Author: Zmuidzinas J.,Gao J.-R., Lowe, I, Ade, P, Ashton, P, Austermann, J, Coppi, G, Cox, E, Devlin, M, Dober, B, Fanfani, V, Fissel, L, Galitzki, N, Gao, J, Gordon, S, Groppi, C, Hilton, G, Hubmayr, J, Klein, J, Li, D, Lourie, N, Mani, H, Mauskopf, P, Mckenney, C, Nati, F, Novak, G, Pisano, G, Romualdez, J, Soler, J, Sinclair, A, Tucker, C, Ullom, J, Vissers, M, Wheeler, C, Williams, P, Lowe I., Ade P. A. R., Ashton P. C., Austermann J. E., Coppi G., Cox E. G., Devlin M. J., Dober B. J., Fanfani V., Fissel L. M., Galitzki N., Gao J., Gordon S., Groppi C. E., Hilton G. C., Hubmayr J., Klein J., Li D., Lourie N. P., Mani H., Mauskopf P., McKenney C., Nati F., Novak G., Pisano G., Romualdez J., Soler J. D., Sinclair A., Tucker C., Ullom J., Vissers M., Wheeler C., Williams P. A., Zmuidzinas J.,Gao J.-R., Lowe, I, Ade, P, Ashton, P, Austermann, J, Coppi, G, Cox, E, Devlin, M, Dober, B, Fanfani, V, Fissel, L, Galitzki, N, Gao, J, Gordon, S, Groppi, C, Hilton, G, Hubmayr, J, Klein, J, Li, D, Lourie, N, Mani, H, Mauskopf, P, Mckenney, C, Nati, F, Novak, G, Pisano, G, Romualdez, J, Soler, J, Sinclair, A, Tucker, C, Ullom, J, Vissers, M, Wheeler, C, Williams, P, Lowe I., Ade P. A. R., Ashton P. C., Austermann J. E., Coppi G., Cox E. G., Devlin M. J., Dober B. J., Fanfani V., Fissel L. M., Galitzki N., Gao J., Gordon S., Groppi C. E., Hilton G. C., Hubmayr J., Klein J., Li D., Lourie N. P., Mani H., Mauskopf P., McKenney C., Nati F., Novak G., Pisano G., Romualdez J., Soler J. D., Sinclair A., Tucker C., Ullom J., Vissers M., Wheeler C., and Williams P. A.
Abstract: The Next Generation Balloon-borne Large Aperture Submillimeter Telescope (BLAST-TNG) is a submillimeter polarimeter designed to map interstellar dust and galactic foregrounds at 250, 350, and 500 microns during a 24-day Antarctic flight. The BLAST-TNG detector arrays are comprised of 918, 469, and 272 MKID pixels, respectively. The pixels are formed from two orthogonally oriented, crossed, linear-polarization sensitive MKID antennae. The arrays are cooled to sub 300 mK temperatures and stabilized via a closed cycle 3He sorption fridge in combination with a 4He vacuum pot. The detectors are read out through a combination of the second-generation Reconfigurable Open Architecture Computing Hardware (ROACH2) and custom RF electronics designed for BLAST-TNG. The firmware and software designed to readout and characterize these detectors was built from scratch by the BLAST team around these detectors, and has been adapted for use by other MKID instruments such as TolTEC and OLIMPO.1 We present an overview of these systems as well as in-depth methodology of the ground-based characterization and the measured in-flight performance.
Published: 2020

24. Linking the dust and chemical evolution: Taurus and Perseus -- New collisional rates for HCN, HNC, and their C, N, and H isotopologues

Author: Navarro-Almaida, D., Bop, C. T., Lique, F., Esplugues, G., Rodríguez-Baras, M., Kramer, C., Romero, C. E., Fuente, A., Caselli, P., Riviére-Marichalar, P., Kirk, J. M., Chacón-Tanarro, A., Roueff, E., Mroczkowski, T., Bhandarkar, T., Devlin, M., Dicker, S., Lowe, I., Mason, B., Sarazin, C. L., Sievers, J., Navarro-Almaida, D., Bop, C. T., Lique, F., Esplugues, G., Rodríguez-Baras, M., Kramer, C., Romero, C. E., Fuente, A., Caselli, P., Riviére-Marichalar, P., Kirk, J. M., Chacón-Tanarro, A., Roueff, E., Mroczkowski, T., Bhandarkar, T., Devlin, M., Dicker, S., Lowe, I., Mason, B., Sarazin, C. L., and Sievers, J.
Abstract: HCN, HNC, and their isotopologues are ubiquitous molecules that can serve as chemical thermometers and evolutionary tracers to characterize star-forming regions. Despite their importance in carrying information that is vital to studies of the chemistry and evolution of star-forming regions, the collision rates of some of these molecules have not been available for rigorous studies in the past. We perform an up-to-date gas and dust chemical characterization of two different star-forming regions, TMC 1-C and NGC 1333-C7, using new collisional rates of HCN, HNC, and their isotopologues. We investigated the possible effects of the environment and stellar feedback in their chemistry and their evolution. With millimeter observations, we derived their column densities, the C and N isotopic fractions, the isomeric ratios, and the deuterium fractionation. The continuum data at 3 mm and 850 $\mu$m allowed us to compute the emissivity spectral index and look for grain growth as an evolutionary tracer. The H$^{13}$CN/HN$^{13}$C ratio is anticorrelated with the deuterium fraction of HCN, thus it can readily serve as a proxy for the temperature. The spectral index $(\beta\sim 1.34-2.09)$ shows a tentative anticorrelation with the H$^{13}$CN/HN$^{13}$C ratio, suggesting grain growth in the evolved, hotter, and less deuterated sources. Unlike TMC 1-C, the south-to-north gradient in dust temperature and spectral index observed in NGC 1333-C7 suggests feedback from the main NGC 1333 cloud. With this up-to-date characterization of two star-forming regions, we found that the chemistry and the physical properties are tightly related. The dust temperature, deuterium fraction, and the spectral index are complementary evolutionary tracers. The large-scale environmental factors may dominate the chemistry and evolution in clustered star-forming regions., Comment: 25 pages, 20 figures
Published: 2022
Full Text: View/download PDF

25. Measurement of the splashback feature around SZ-selected Galaxy clusters with DES, SPT, and ACT

Author: Shin, T, Adhikari, S, Baxter, E, Chang, C, Jain, B, Battaglia, N, Bleem, L, Bocquet, S, Derose, J, Gruen, D, Hilton, M, Kravtsov, A, Mcclintock, T, Rozo, E, Rykoff, E, Varga, T, Wechsler, R, Wu, H, Zhang, Z, Aiola, S, Allam, S, Bechtol, K, Benson, B, Bertin, E, Bond, J, Brodwin, M, Brooks, D, Buckley-Geer, E, Burke, D, Carlstrom, J, Rosell, A, Kind, M, Carretero, J, Castander, F, Choi, S, Cunha, C, Crawford, T, Da Costa, L, De Vicente, J, Desai, S, Devlin, M, Dietrich, J, Doel, P, Dunkley, J, Eifler, T, Evrard, A, Flaugher, B, Fosalba, P, Gallardo, P, Garcia-Bellido, J, Gaztanaga, E, Gerdes, D, Gralla, M, Gruendl, R, Gschwend, J, Gupta, N, Gutierrez, G, Hartley, W, Hill, J, Ho, S, Hollowood, D, Honscheid, K, Hoyle, B, Huffenberger, K, Hughes, J, James, D, Jeltema, T, Kim, A, Krause, E, Kuehn, K, Lahav, O, Lima, M, Madhavacheril, M, Maia, M, Marshall, J, Maurin, L, Mcmahon, J, Menanteau, F, Miller, C, Miquel, R, Mohr, J, Naess, S, Nati, F, Newburgh, L, Niemack, M, Ogando, R, Page, L, Partridge, B, Patil, S, Plazas, A, Rapetti, D, Reichardt, C, Romer, A, Sanchez, E, Scarpine, V, Schindler, R, Serrano, S, Smith, M, Smith, R, Soares-Santos, M, Sobreira, F, Staggs, S, Stark, A, Stein, G, Suchyta, E, Swanson, M, Tarle, G, Thomas, D, Van Engelen, A, Wollack, E, Xu, Z, Shin T., Adhikari S., Baxter E. J., Chang C., Jain B., Battaglia N., Bleem L., Bocquet S., DeRose J., Gruen D., Hilton M., Kravtsov A., McClintock T., Rozo E., Rykoff E. S., Varga T. N., Wechsler R. H., Wu H., Zhang Z., Aiola S., Allam S., Bechtol K., Benson B. A., Bertin E., Bond J. R., Brodwin M., Brooks D., Buckley-Geer E., Burke D. L., Carlstrom J. E., Rosell A., Kind M., Carretero J., Castander F. J., Choi S. K., Cunha C. E., Crawford T. M., Da Costa L. N., De Vicente J., Desai S., Devlin M. J., Dietrich J. P., Doel P., Dunkley J., Eifler T. F., Evrard A. E., Flaugher B., Fosalba P., Gallardo P. A., Garcia-Bellido J., Gaztanaga E., Gerdes D. W., Gralla M., Gruendl R. A., Gschwend J., Gupta N., Gutierrez G., Hartley W. G., Hill J. C., Ho S. P., Hollowood D. L., Honscheid K., Hoyle B., Huffenberger K., Hughes J. P., James D. J., Jeltema T., Kim A. G., Krause E., Kuehn K., Lahav O., Lima M., Madhavacheril M. S., Maia M. A. G., Marshall J. L., Maurin L., McMahon J., Menanteau F., Miller C. J., Miquel R., Mohr J. J., Naess S., Nati F., Newburgh L., Niemack M. D., Ogando R. L. C., Page L. A., Partridge B., Patil S., Plazas A. A., Rapetti D., Reichardt C. L., Romer A. K., Sanchez E., Scarpine V., Schindler R., Serrano S., Smith M., Smith R. C., Soares-Santos M., Sobreira F., Staggs S. T., Stark A., Stein G., Suchyta E., Swanson M. E. C., Tarle G., Thomas D., Van Engelen A., Wollack E. J., Xu Z., Shin, T, Adhikari, S, Baxter, E, Chang, C, Jain, B, Battaglia, N, Bleem, L, Bocquet, S, Derose, J, Gruen, D, Hilton, M, Kravtsov, A, Mcclintock, T, Rozo, E, Rykoff, E, Varga, T, Wechsler, R, Wu, H, Zhang, Z, Aiola, S, Allam, S, Bechtol, K, Benson, B, Bertin, E, Bond, J, Brodwin, M, Brooks, D, Buckley-Geer, E, Burke, D, Carlstrom, J, Rosell, A, Kind, M, Carretero, J, Castander, F, Choi, S, Cunha, C, Crawford, T, Da Costa, L, De Vicente, J, Desai, S, Devlin, M, Dietrich, J, Doel, P, Dunkley, J, Eifler, T, Evrard, A, Flaugher, B, Fosalba, P, Gallardo, P, Garcia-Bellido, J, Gaztanaga, E, Gerdes, D, Gralla, M, Gruendl, R, Gschwend, J, Gupta, N, Gutierrez, G, Hartley, W, Hill, J, Ho, S, Hollowood, D, Honscheid, K, Hoyle, B, Huffenberger, K, Hughes, J, James, D, Jeltema, T, Kim, A, Krause, E, Kuehn, K, Lahav, O, Lima, M, Madhavacheril, M, Maia, M, Marshall, J, Maurin, L, Mcmahon, J, Menanteau, F, Miller, C, Miquel, R, Mohr, J, Naess, S, Nati, F, Newburgh, L, Niemack, M, Ogando, R, Page, L, Partridge, B, Patil, S, Plazas, A, Rapetti, D, Reichardt, C, Romer, A, Sanchez, E, Scarpine, V, Schindler, R, Serrano, S, Smith, M, Smith, R, Soares-Santos, M, Sobreira, F, Staggs, S, Stark, A, Stein, G, Suchyta, E, Swanson, M, Tarle, G, Thomas, D, Van Engelen, A, Wollack, E, Xu, Z, Shin T., Adhikari S., Baxter E. J., Chang C., Jain B., Battaglia N., Bleem L., Bocquet S., DeRose J., Gruen D., Hilton M., Kravtsov A., McClintock T., Rozo E., Rykoff E. S., Varga T. N., Wechsler R. H., Wu H., Zhang Z., Aiola S., Allam S., Bechtol K., Benson B. A., Bertin E., Bond J. R., Brodwin M., Brooks D., Buckley-Geer E., Burke D. L., Carlstrom J. E., Rosell A., Kind M., Carretero J., Castander F. J., Choi S. K., Cunha C. E., Crawford T. M., Da Costa L. N., De Vicente J., Desai S., Devlin M. J., Dietrich J. P., Doel P., Dunkley J., Eifler T. F., Evrard A. E., Flaugher B., Fosalba P., Gallardo P. A., Garcia-Bellido J., Gaztanaga E., Gerdes D. W., Gralla M., Gruendl R. A., Gschwend J., Gupta N., Gutierrez G., Hartley W. G., Hill J. C., Ho S. P., Hollowood D. L., Honscheid K., Hoyle B., Huffenberger K., Hughes J. P., James D. J., Jeltema T., Kim A. G., Krause E., Kuehn K., Lahav O., Lima M., Madhavacheril M. S., Maia M. A. G., Marshall J. L., Maurin L., McMahon J., Menanteau F., Miller C. J., Miquel R., Mohr J. J., Naess S., Nati F., Newburgh L., Niemack M. D., Ogando R. L. C., Page L. A., Partridge B., Patil S., Plazas A. A., Rapetti D., Reichardt C. L., Romer A. K., Sanchez E., Scarpine V., Schindler R., Serrano S., Smith M., Smith R. C., Soares-Santos M., Sobreira F., Staggs S. T., Stark A., Stein G., Suchyta E., Swanson M. E. C., Tarle G., Thomas D., Van Engelen A., Wollack E. J., and Xu Z.
Abstract: We present a detection of the splashback feature around galaxy clusters selected using the Sunyaev-Zel'dovich (SZ) signal. Recent measurements of the splashback feature around optically selected galaxy clusters have found that the splashback radius, rsp, is smaller than predicted by N-body simulations. Apossible explanation for this discrepancy is that rsp inferred from the observed radial distribution of galaxies is affected by selection effects related to the optical cluster-finding algorithms. We test this possibility by measuring the splashback feature in clusters selected via the SZ effect in data from the South Pole Telescope SZ survey and the Atacama Cosmology Telescope Polarimeter survey. The measurement is accomplished by correlating these cluster samples with galaxies detected in the Dark Energy Survey Year 3 data. The SZ observable used to select clusters in this analysis is expected to have a tighter correlation with halo mass and to be more immune to projection effects and aperture-induced biases, potentially ameliorating causes of systematic error for optically selected clusters. We find that the measured r(sp) for SZ-selected clusters is consistent with the expectations from simulations, although the small number of SZ-selected clusters makes a precise comparison difficult. In agreement with previous work, when using optically selected redMaPPer clusters with similar mass and redshift distributions, r(sp) is similar to 2 sigma smaller than in the simulations. These results motivate detailed investigations of selection biases in optically selected cluster catalogues and exploration of the splashback feature around larger samples of SZ-selected clusters. Additionally, we investigate trends in the galaxy profile and splashback feature as a function of galaxy colour, finding that blue galaxies have profiles close to a power law with no discernible splashback feature, which is consistent with them being on their first infall into the cluster.
Published: 2019

26. The atacama cosmology telescope: Two-season ACTPol extragalactic point sources and their polarization properties

Author: Datta, R, Aiola, S, Choi, S, Devlin, M, Dunkley, J, Dunner, R, Gallardo, P, Gralla, M, Halpern, M, Hasselfield, M, Hilton, M, Hincks, A, Ho, S, Hubmayr, J, Huffenberger, K, Hughes, J, Kosowsky, A, Lopez-Caraballo, C, Louis, T, Lungu, M, Marriage, T, Maurin, L, Mcmahon, J, Moodley, K, Naess, S, Nati, F, Niemack, M, Page, L, Partridge, B, Prince, H, Staggs, S, Switzer, E, Wollack, E, Farren, G, Datta R., Aiola S., Choi S. K., Devlin M., Dunkley J., Dunner R., Gallardo P. A., Gralla M., Halpern M., Hasselfield M., Hilton M., Hincks A. D., Ho S. -P. P., Hubmayr J., Huffenberger K. M., Hughes J. P., Kosowsky A., Lopez-Caraballo C. H., Louis T., Lungu M., Marriage T., Maurin L., McMahon J., Moodley K., Naess S. K., Nati F., Niemack M. D., Page L. A., Partridge B., Prince H., Staggs S. T., Switzer E. R., Wollack E. J., Farren G., Datta, R, Aiola, S, Choi, S, Devlin, M, Dunkley, J, Dunner, R, Gallardo, P, Gralla, M, Halpern, M, Hasselfield, M, Hilton, M, Hincks, A, Ho, S, Hubmayr, J, Huffenberger, K, Hughes, J, Kosowsky, A, Lopez-Caraballo, C, Louis, T, Lungu, M, Marriage, T, Maurin, L, Mcmahon, J, Moodley, K, Naess, S, Nati, F, Niemack, M, Page, L, Partridge, B, Prince, H, Staggs, S, Switzer, E, Wollack, E, Farren, G, Datta R., Aiola S., Choi S. K., Devlin M., Dunkley J., Dunner R., Gallardo P. A., Gralla M., Halpern M., Hasselfield M., Hilton M., Hincks A. D., Ho S. -P. P., Hubmayr J., Huffenberger K. M., Hughes J. P., Kosowsky A., Lopez-Caraballo C. H., Louis T., Lungu M., Marriage T., Maurin L., McMahon J., Moodley K., Naess S. K., Nati F., Niemack M. D., Page L. A., Partridge B., Prince H., Staggs S. T., Switzer E. R., Wollack E. J., and Farren G.
Abstract: We report on measurements of the polarization of extragalactic sources at.148 GHz made during the first two seasons of the Atacama Cosmology Telescope Polarization (ACTPol) survey. The survey covered 680 deg(2) of the sky on the celestial equator. Polarization measurements of 169 intensity-selected sources brighter than 30 mJy, that are predominantly active galactic nuclei, are presented. Above a total flux of 215 mJy where the noise bias removal in the polarization measurement is reliable, we detect 2.6 sources, 14 of which have a detection of linear polarization at greater than 3 sigma-significance. The distribution of the fractional polarization as a function of total source intensity is analysed. Our result is consistent with the scenario that the fractional polarization of our measured radio source population is independent of total intensity down to the limits of our measurements and well described by a Gaussian distribution with a mean fractional polarization p(m) = 0.02.8 +/- 0.005 and standard deviation sigma(pm) = 0.054, truncated at p = 0. Extrapolating this model for the distribution of source polarization below the ACTPol detection threshold, we predict: that one could get a clean measure of the E mode polarization power spectrum. of the microwave background out to l approximate to 6000 with 1 HK-arcminute maps over 10% of the sky from a future stu-vey. We also study the spectral energy distribution of the total and polarized source flux densities by cross-matching with low.radio frequency catalogues. We do not find any correlation between the spectral indices for total flux and polarized flux.
Published: 2019

27. Preclinical small molecule WEHI-7326 overcomes drug resistance and elicits response in patient-derived xenograft models of human treatment-refractory tumors

Author: Grohmann, C, Walker, F, Devlin, M, Luo, MX, Chüeh, AC, Doherty, J, Vaillant, F, Ho, GY, Wakefield, MJ, Weeden, CE, Kamili, A, Murray, J, Po’uha, ST, Weinstock, J, Kane, SR, Faux, MC, Broekhuizen, E, Zheng, Y, Shield-Artin, K, Kershaw, NJ, Tan, CW, Witchard, HM, Ebert, G, Charman, SA, Street, I, Kavallaris, M, Haber, M, Fletcher, JI, Asselin-Labat, ML, Scott, CL, Visvader, JE, Lindeman, GJ, Watson, KG, Burgess, AW, Lessene, G, Grohmann, C, Walker, F, Devlin, M, Luo, MX, Chüeh, AC, Doherty, J, Vaillant, F, Ho, GY, Wakefield, MJ, Weeden, CE, Kamili, A, Murray, J, Po’uha, ST, Weinstock, J, Kane, SR, Faux, MC, Broekhuizen, E, Zheng, Y, Shield-Artin, K, Kershaw, NJ, Tan, CW, Witchard, HM, Ebert, G, Charman, SA, Street, I, Kavallaris, M, Haber, M, Fletcher, JI, Asselin-Labat, ML, Scott, CL, Visvader, JE, Lindeman, GJ, Watson, KG, Burgess, AW, and Lessene, G
Abstract: Targeting cell division by chemotherapy is a highly effective strategy to treat a wide range of cancers. However, there are limitations of many standard-of-care chemotherapies: undesirable drug toxicity, side-effects, resistance and high cost. New small molecules which kill a wide range of cancer subtypes, with good therapeutic window in vivo, have the potential to complement the current arsenal of anti-cancer agents and deliver improved safety profiles for cancer patients. We describe results with a new anti-cancer small molecule, WEHI-7326, which causes cell cycle arrest in G2/M, cell death in vitro, and displays efficacious anti-tumor activity in vivo. WEHI-7326 induces cell death in a broad range of cancer cell lines, including taxane-resistant cells, and inhibits growth of human colon, brain, lung, prostate and breast tumors in mice xenografts. Importantly, the compound elicits tumor responses as a single agent in patient-derived xenografts of clinically aggressive, treatment-refractory neuroblastoma, breast, lung and ovarian cancer. In combination with standard-of-care, WEHI-7326 induces a remarkable complete response in a mouse model of high-risk neuroblastoma. WEHI-7326 is mechanistically distinct from known microtubule-targeting agents and blocks cells early in mitosis to inhibit cell division, ultimately leading to apoptotic cell death. The compound is simple to produce and possesses favorable pharmacokinetic and toxicity profiles in rodents. It represents a novel class of anti-cancer therapeutics with excellent potential for further development due to the ease of synthesis, simple formulation, moderate side effects and potent in vivo activity. WEHI-7326 has the potential to complement current frontline anti-cancer drugs and to overcome drug resistance in a wide range of cancers.
Published: 2021

28. Thermodynamic evolution of the $z=1.75$ galaxy cluster IDCS J1426.5+3508

Author: Andreon, S., Romero, C., Castagna, F., Ragagnin, A., Devlin, M., Dicker, S., Mason, B., Mroczkowski, T., Sarazin, C., Sievers, J., Stanchfield, S., Andreon, S., Romero, C., Castagna, F., Ragagnin, A., Devlin, M., Dicker, S., Mason, B., Mroczkowski, T., Sarazin, C., Sievers, J., and Stanchfield, S.
Abstract: We present resolved thermodynamic profiles out to 500 kpc, about $r_{500}$, of the $z=1.75$ galaxy cluster IDCS J1426.5+3508 with 40 kpc resolution. Thanks to the combination of Sunyaev-Zel'dovich and X-ray datasets, IDCS J1426.5+3508 becomes the most distant cluster with resolved thermodynamic profiles. These are derived assuming a non-parametric pressure profile and a very flexible model for the electron density profile. The shape of the pressure profile is flatter than the universal pressure profile. The IDCS J1426.5+3508 temperature profile is increasing radially out to 500 kpc. To identify the possible future evolution of IDCS J1426.5+3508 , we compared it with its local descendants that numerical simulations show to be $0.65\pm0.12$ dex more massive. We found no evolution at 30 kpc, indicating a fine tuning between cooling and heating at small radii. At $30
Published: 2021
Full Text: View/download PDF

29. The mass and galaxy distribution around SZ-selected clusters

Author: Shin, T., Jain, B., Adhikari, S., Baxter, E. J., Chang, C., Pandey, S., Salcedo, A., Weinberg, D. H., Amsellem, A., Battaglia, N., Belyakov, M., Dacunha, T., Goldstein, S., Kravtsov, A. V., Varga, T. N., Abbott, T. M. C., Aguena, M., Alarcon, A., Allam, S., Amon, A., Andrade-Oliveira, F., Annis, J., Bacon, D., Bechtol, K., Becker, M. R., Bernstein, G. M., Bertin, E., Bocquet, S., Bond, J. R., Brooks, D., Buckley-Geer, E., Burke, D. L., Campos, A., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Chen, R., Choi, A., Costanzi, M., da Costa, L. N., DeRose, J., Desai, S., De Vicente, J., Devlin, M. J., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Doux, C., Drlica-Wagner, A., Eckert, K., Elvin-Poole, J., Everett, S., Ferraro, S., Ferrero, I., Ferté, A., Flaugher, B., Frieman, J., Gallardo, P. A., Gatti, M., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., Harrison, I., Hartley, W. G., Hill, J. C., Hilton, M., Hinton, S. R., Hollowood, D. L., Hughes, J. P., James, D. J., Jarvis, M., Jeltema, T., Koopman, B. J., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Lokken, M., MacCrann, N., Madhavacheril, M. S., Maia, M. A. G., McCullough, J., McMahon, J., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Moodley, K., Morgan, R., Myles, J., Nati, F., Navarro-Alsina, A., Niemack, M. D., Ogando, R. L. C., Page, L. A., Palmese, A., Partridge, B., Paz-Chinchón, F., Pereira, M. E. S., Pieres, A., Malagón, A. A. Plazas, Prat, J., Raveri, M., Rodriguez-Monroy, M., Rollins, R. P., Romer, A. K., Rykoff, E. S., Salatino, M., Sánchez, C., Sanchez, E., Santiago, B., Scarpine, V., Schillaci, A., Secco, L. F., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Sherwin, B. D., Sifón, C., Smith, M., Soares-Santos, M., Staggs, S. T., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Troxel, M. A., Tutusaus, I., Vavagiakis, E. M., Weller, J., Wollack, E. J., Yanny, B., Yin, B., Zhang, Y., Shin, T., Jain, B., Adhikari, S., Baxter, E. J., Chang, C., Pandey, S., Salcedo, A., Weinberg, D. H., Amsellem, A., Battaglia, N., Belyakov, M., Dacunha, T., Goldstein, S., Kravtsov, A. V., Varga, T. N., Abbott, T. M. C., Aguena, M., Alarcon, A., Allam, S., Amon, A., Andrade-Oliveira, F., Annis, J., Bacon, D., Bechtol, K., Becker, M. R., Bernstein, G. M., Bertin, E., Bocquet, S., Bond, J. R., Brooks, D., Buckley-Geer, E., Burke, D. L., Campos, A., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Chen, R., Choi, A., Costanzi, M., da Costa, L. N., DeRose, J., Desai, S., De Vicente, J., Devlin, M. J., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Doux, C., Drlica-Wagner, A., Eckert, K., Elvin-Poole, J., Everett, S., Ferraro, S., Ferrero, I., Ferté, A., Flaugher, B., Frieman, J., Gallardo, P. A., Gatti, M., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., Harrison, I., Hartley, W. G., Hill, J. C., Hilton, M., Hinton, S. R., Hollowood, D. L., Hughes, J. P., James, D. J., Jarvis, M., Jeltema, T., Koopman, B. J., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Lokken, M., MacCrann, N., Madhavacheril, M. S., Maia, M. A. G., McCullough, J., McMahon, J., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Moodley, K., Morgan, R., Myles, J., Nati, F., Navarro-Alsina, A., Niemack, M. D., Ogando, R. L. C., Page, L. A., Palmese, A., Partridge, B., Paz-Chinchón, F., Pereira, M. E. S., Pieres, A., Malagón, A. A. Plazas, Prat, J., Raveri, M., Rodriguez-Monroy, M., Rollins, R. P., Romer, A. K., Rykoff, E. S., Salatino, M., Sánchez, C., Sanchez, E., Santiago, B., Scarpine, V., Schillaci, A., Secco, L. F., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Sherwin, B. D., Sifón, C., Smith, M., Soares-Santos, M., Staggs, S. T., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Troxel, M. A., Tutusaus, I., Vavagiakis, E. M., Weller, J., Wollack, E. J., Yanny, B., Yin, B., and Zhang, Y.
Abstract: We present measurements of the radial profiles of the mass and galaxy number density around Sunyaev-Zel'dovich-selected clusters using both weak lensing and galaxy counts. The clusters are selected from the Atacama Cosmology Telescope Data Release 5 and the galaxies from the Dark Energy Survey Year 3 dataset. With signal-to-noise of 62 (43) for galaxy (weak lensing) profiles over scales of about $0.2-20h^{-1}$ Mpc, these are the highest precision measurements for SZ-selected clusters to date. Because SZ selection closely approximates mass selection, these measurements enable several tests of theoretical models of the mass and light distribution around clusters. Our main findings are: 1. The splashback feature is detected at a consistent location in both the mass and galaxy profiles and its location is consistent with predictions of cold dark matter N-body simulations. 2. The full mass profile is also consistent with the simulations; hence it can constrain alternative dark matter models that modify the mass distribution of clusters. 3. The shapes of the galaxy and lensing profiles are remarkably similar for our sample over the entire range of scales, from well inside the cluster halo to the quasilinear regime. This can be used to constrain processes such as quenching and tidal disruption that alter the galaxy distribution inside the halo, and scale-dependent features in the transition regime outside the halo. We measure the dependence of the profile shapes on the galaxy sample, redshift and cluster mass. We extend the Diemer \& Kravtsov model for the cluster profiles to the linear regime using perturbation theory and show that it provides a good match to the measured profiles. We also compare the measured profiles to predictions of the standard halo model and simulations that include hydrodynamics. Applications of these results to cluster mass estimation and cosmology are discussed., Comment: 15 pages, 6 figures (main) + 3 pages, 6 figures (appendix), submitted to MNRAS
Published: 2021
Full Text: View/download PDF

30. Student Success in a Global Pandemic

Author: Devlin, M, Mckay, Jade, Devlin, M, and Mckay, Jade
Abstract: The catastrophic disruption to higher education from the COVID-19 pandemic has brought about significant and rapid changes to the delivery of mainstream teaching and learning in higher education institutions around the globe, in particular through the use of online learning. The many examples of innovation and novelty demonstrated by institutions and individuals in their support of students and their learning provides a timely opportunity for the sharing of exemplary activities and outcomes in the Student Success Journal. We are pleased to announce that Student Success in a Global Pandemic has been chosen as the topic for the 2021 Special Issue to enable academics, practitioners, leaders and policy makers to share their stories and outcomes and have ongoing learning from a time of extraordinary innovation.
Published: 2021

31. Probing Galaxy Evolution in Massive Clusters Using ACT and DES: Splashback as a Cosmic Clock

Author: Adhikari, S, Adhikari, S, Shin, TH, Jain, B, Hilton, M, Baxter, E, Chang, C, Wechsler, RH, Battaglia, N, Bond, JR, Bocquet, S, Choi, SK, Derose, J, Devlin, M, Dunkley, J, Evrard, AE, Ferraro, S, Hill, JC, Hughes, JP, Gallardo, PA, Lokken, M, Macinnis, A, Madhavacheril, MS, McMahon, J, Nati, F, Newburgh, LB, Niemack, MD, Page, LA, Palmese, A, Partridge, B, Rozo, E, Rykoff, E, Salatino, M, Schillaci, A, Sehgal, N, Sifón, C, To, CH, Wollack, E, Wu, HY, Xu, Z, Aguena, M, Allam, S, Amon, A, Annis, J, Avila, S, Bacon, D, Bertin, E, Bhargava, S, Brooks, D, Burke, DL, Rosell, AC, Kind, MC, Carretero, J, Castander, FJ, Choi, A, Costanzi, M, Da Costa, LN, Vicente, JD, Desai, S, Diehl, TH, Doel, P, Everett, S, Ferrero, I, Ferté, A, Flaugher, B, Fosalba, P, Frieman, J, García-Bellido, J, Gaztanaga, E, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Hartley, WG, Hinton, SR, Hollowood, DL, Honscheid, K, James, DJ, Jeltema, T, Kuehn, K, Kuropatkin, N, Lahav, O, Lima, M, Maia, MAG, Marshall, JL, Martini, P, Melchior, P, Menanteau, F, Miquel, R, Morgan, R, L. C. Ogando, R, Paz-Chinchón, F, Malagón, AP, Sanchez, E, Santiago, B, Scarpine, V, Serrano, S, Sevilla-Noarbe, I, Smith, M, Soares-Santos, M, Suchyta, E, Adhikari, S, Adhikari, S, Shin, TH, Jain, B, Hilton, M, Baxter, E, Chang, C, Wechsler, RH, Battaglia, N, Bond, JR, Bocquet, S, Choi, SK, Derose, J, Devlin, M, Dunkley, J, Evrard, AE, Ferraro, S, Hill, JC, Hughes, JP, Gallardo, PA, Lokken, M, Macinnis, A, Madhavacheril, MS, McMahon, J, Nati, F, Newburgh, LB, Niemack, MD, Page, LA, Palmese, A, Partridge, B, Rozo, E, Rykoff, E, Salatino, M, Schillaci, A, Sehgal, N, Sifón, C, To, CH, Wollack, E, Wu, HY, Xu, Z, Aguena, M, Allam, S, Amon, A, Annis, J, Avila, S, Bacon, D, Bertin, E, Bhargava, S, Brooks, D, Burke, DL, Rosell, AC, Kind, MC, Carretero, J, Castander, FJ, Choi, A, Costanzi, M, Da Costa, LN, Vicente, JD, Desai, S, Diehl, TH, Doel, P, Everett, S, Ferrero, I, Ferté, A, Flaugher, B, Fosalba, P, Frieman, J, García-Bellido, J, Gaztanaga, E, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Hartley, WG, Hinton, SR, Hollowood, DL, Honscheid, K, James, DJ, Jeltema, T, Kuehn, K, Kuropatkin, N, Lahav, O, Lima, M, Maia, MAG, Marshall, JL, Martini, P, Melchior, P, Menanteau, F, Miquel, R, Morgan, R, L. C. Ogando, R, Paz-Chinchón, F, Malagón, AP, Sanchez, E, Santiago, B, Scarpine, V, Serrano, S, Sevilla-Noarbe, I, Smith, M, Soares-Santos, M, and Suchyta, E
Abstract: We measure the projected number density profiles of galaxies and the splashback feature in clusters selected by the Sunyaev-Zel'dovich effect from the Advanced Atacama Cosmology Telescope (AdvACT) survey using galaxies observed by the Dark Energy Survey (DES). The splashback radius is consistent with CDM-only simulations and is located at 2.4-0.4+0.3 Mpc h-1. We split the galaxies on color and find significant differences in their profile shapes. Red and green-valley galaxies show a splashback-like minimum in their slope profile consistent with theory, while the bluest galaxies show a weak feature at a smaller radius. We develop a mapping of galaxies to subhalos in simulations and assign colors based on infall time onto their hosts. We find that the shift in location of the steepest slope and different profile shapes can be mapped to the average time of infall of galaxies of different colors. The steepest slope traces a discontinuity in the phase space of dark matter halos. By relating spatial profiles to infall time, we can use splashback as a clock to understand galaxy quenching. We find that red galaxies have on average been in clusters over 3.2 Gyr, green galaxies about 2.2 Gyr, while blue galaxies have been accreted most recently and have not reached apocenter. Using the full radial profiles, we fit a simple quenching model and find that the onset of galaxy quenching occurs after a delay of about a gigayear and that galaxies quench rapidly thereafter with an exponential timescale of 0.6 Gyr.
Published: 2021

32. The Atacama Cosmology Telescope: Microwave Intensity and Polarization Maps of the Galactic Center

Author: Guan, Y, Guan, Y, Clark, SE, Hensley, BS, Gallardo, PA, Naess, S, Duell, CJ, Aiola, S, Atkins, Z, Calabrese, E, Choi, SK, Cothard, NF, Devlin, M, Duivenvoorden, AJ, Dunkley, J, Dünner, R, Ferraro, S, Hasselfield, M, Hughes, JP, Koopman, BJ, Kosowsky, AB, Madhavacheril, MS, McMahon, J, Nati, F, Niemack, MD, Page, LA, Salatino, M, Schaan, E, Sehgal, N, Sifón, C, Staggs, S, Vavagiakis, EM, Wollack, EJ, Xu, Z, Guan, Y, Guan, Y, Clark, SE, Hensley, BS, Gallardo, PA, Naess, S, Duell, CJ, Aiola, S, Atkins, Z, Calabrese, E, Choi, SK, Cothard, NF, Devlin, M, Duivenvoorden, AJ, Dunkley, J, Dünner, R, Ferraro, S, Hasselfield, M, Hughes, JP, Koopman, BJ, Kosowsky, AB, Madhavacheril, MS, McMahon, J, Nati, F, Niemack, MD, Page, LA, Salatino, M, Schaan, E, Sehgal, N, Sifón, C, Staggs, S, Vavagiakis, EM, Wollack, EJ, and Xu, Z
Abstract: We present arcminute-resolution intensity and polarization maps of the Galactic center made with the Atacama Cosmology Telescope. The maps cover a 32 deg2 field at 98, 150, and 224 GHz with |l| ≤ 4 , |b| ≤ 2 . We combine these data with Planck observations at similar frequencies to create coadded maps with increased sensitivity at large angular scales. With the coadded maps, we are able to resolve many known features of the Central Molecular Zone (CMZ) in both total intensity and polarization. We map the orientation of the plane-of-sky component of the Galactic magnetic field inferred from the polarization angle in the CMZ, finding significant changes in morphology in the three frequency bands as the underlying dominant emission mechanism changes from synchrotron to dust emission. Selected Galactic center sources, including Sgr A∗, the Brick molecular cloud (G0.253+0.016), the Mouse pulsar wind nebula (G359.23-0.82), and the Tornado supernova remnant candidate (G357.7-0.1), are examined in detail. These data illustrate the potential for leveraging ground-based cosmic microwave background polarization experiments for Galactic science.
Published: 2021

33. The Atacama Cosmology Telescope: A Search for Planet 9

Author: Naess, S, Naess, S, Aiola, S, Battaglia, N, Bond, RJ, Calabrese, E, Choi, SK, Cothard, NF, Halpern, M, Hill, JC, Koopman, BJ, Devlin, M, McMahon, J, Dicker, S, Duivenvoorden, AJ, Dunkley, J, Fanfani, V, Ferraro, S, Gallardo, PA, Guan, Y, Han, D, Hasselfield, M, Hincks, AD, Huffenberger, K, Kosowsky, AB, Louis, T, Macinnis, A, Madhavacheril, MS, Nati, F, Niemack, MD, Page, L, Salatino, M, Schaan, E, Orlowski-Scherer, J, Schillaci, A, Schmitt, B, Sehgal, N, Sifón, C, Staggs, S, Engelen, AV, Wollack, EJ, Naess, S, Naess, S, Aiola, S, Battaglia, N, Bond, RJ, Calabrese, E, Choi, SK, Cothard, NF, Halpern, M, Hill, JC, Koopman, BJ, Devlin, M, McMahon, J, Dicker, S, Duivenvoorden, AJ, Dunkley, J, Fanfani, V, Ferraro, S, Gallardo, PA, Guan, Y, Han, D, Hasselfield, M, Hincks, AD, Huffenberger, K, Kosowsky, AB, Louis, T, Macinnis, A, Madhavacheril, MS, Nati, F, Niemack, MD, Page, L, Salatino, M, Schaan, E, Orlowski-Scherer, J, Schillaci, A, Schmitt, B, Sehgal, N, Sifón, C, Staggs, S, Engelen, AV, and Wollack, EJ
Abstract: We use Atacama Cosmology Telescope (ACT) observations at 98 GHz (2015–2019), 150 GHz (2013–2019), and 229 GHz (2017–2019) to perform a blind shift-and-stack search for Planet 9. The search explores distances from 300 au to 2000 au and velocities up to 6.′3 per year, depending on the distance (r). For a 5 Earth-mass Planet 9 the detection limit varies from 325 au to 625 au, depending on the sky location. For a 10 Earth-mass planet the corresponding range is 425 au to 775 au. The predicted aphelion and most likely location of the planet corresponds to the shallower end of these ranges. The search covers the whole 18,000 square degrees of the ACT survey. No significant detections are found, which is used to place limits on the millimeter-wave flux density of Planet 9 over much of its orbit. Overall we eliminate roughly 17% and 9% of the parameter space for a 5 and 10 Earth-mass Planet 9, respectively. These bounds approach those of a recent INPOP19a ephemeris-based analysis, but do not exceed it. We also provide a list of the 10 strongest candidates from the search for possible follow-up. More generally, we exclude (at 95% confidence) the presence of an unknown solar system object within our survey area brighter than 4–12 mJy (depending on position) at 150 GHz with current distance 300 au < r < 600 au and heliocentric angular velocity , corresponding to low-to-moderate eccentricities. These limits worsen gradually beyond 600 au, reaching 5–15 mJy by 1500 au.
Published: 2021

34. Preclinical small molecule WEHI-7326 overcomes drug resistance and elicits response in patient-derived xenograft models of human treatment-refractory tumors

Author: Grohmann, C, Walker, F, Devlin, M, Luo, M-X, Chueh, AC, Doherty, J, Vaillant, F, Ho, G-Y, Wakefield, MJ, Weeden, CE, Kamili, A, Murray, J, Po'uha, ST, Weinstock, J, Kane, SR, Faux, MC, Broekhuizen, E, Zheng, Y, Shield-Artin, K, Kershaw, NJ, Tan, CW, Witchard, HM, Ebert, G, Charman, SA, Street, I, Kavallaris, M, Haber, M, Fletcher, JI, Asselin-Labat, M-L, Scott, CL, Visvader, JE, Lindeman, GJ, Watson, KG, Burgess, AW, Lessene, G, Grohmann, C, Walker, F, Devlin, M, Luo, M-X, Chueh, AC, Doherty, J, Vaillant, F, Ho, G-Y, Wakefield, MJ, Weeden, CE, Kamili, A, Murray, J, Po'uha, ST, Weinstock, J, Kane, SR, Faux, MC, Broekhuizen, E, Zheng, Y, Shield-Artin, K, Kershaw, NJ, Tan, CW, Witchard, HM, Ebert, G, Charman, SA, Street, I, Kavallaris, M, Haber, M, Fletcher, JI, Asselin-Labat, M-L, Scott, CL, Visvader, JE, Lindeman, GJ, Watson, KG, Burgess, AW, and Lessene, G
Abstract: Targeting cell division by chemotherapy is a highly effective strategy to treat a wide range of cancers. However, there are limitations of many standard-of-care chemotherapies: undesirable drug toxicity, side-effects, resistance and high cost. New small molecules which kill a wide range of cancer subtypes, with good therapeutic window in vivo, have the potential to complement the current arsenal of anti-cancer agents and deliver improved safety profiles for cancer patients. We describe results with a new anti-cancer small molecule, WEHI-7326, which causes cell cycle arrest in G2/M, cell death in vitro, and displays efficacious anti-tumor activity in vivo. WEHI-7326 induces cell death in a broad range of cancer cell lines, including taxane-resistant cells, and inhibits growth of human colon, brain, lung, prostate and breast tumors in mice xenografts. Importantly, the compound elicits tumor responses as a single agent in patient-derived xenografts of clinically aggressive, treatment-refractory neuroblastoma, breast, lung and ovarian cancer. In combination with standard-of-care, WEHI-7326 induces a remarkable complete response in a mouse model of high-risk neuroblastoma. WEHI-7326 is mechanistically distinct from known microtubule-targeting agents and blocks cells early in mitosis to inhibit cell division, ultimately leading to apoptotic cell death. The compound is simple to produce and possesses favorable pharmacokinetic and toxicity profiles in rodents. It represents a novel class of anti-cancer therapeutics with excellent potential for further development due to the ease of synthesis, simple formulation, moderate side effects and potent in vivo activity. WEHI-7326 has the potential to complement current frontline anti-cancer drugs and to overcome drug resistance in a wide range of cancers.
Published: 2021

35. The Simons Observatory: modeling optical systematics in the Large Aperture Telescope

Author: Gudmundsson, JE, Gallardo, PA, Puddu, R, Dicker, SR, Adler, AE, Ali, AM, Bazarko, A, Chesmore, GE, Coppi, G, Cothard, NF, Dachlythra, N, Devlin, M, Dunner, R, Fabbian, G, Galitzki, N, Golec, JE, Ho, S-PP, Hargrave, PC, Kofman, AM, Lee, AT, Limon, M, Matsuda, FT, Mauskopf, PD, Moodley, K, Nati, F, Niemack, MD, Orlowski-Scherer, J, Page, LA, Partridge, B, Puglisi, G, Reichardt, CL, Sierra, CE, Simon, SM, Teply, GP, Tucker, C, Wollack, EJ, Xu, Z, Zhu, N, Gudmundsson, JE, Gallardo, PA, Puddu, R, Dicker, SR, Adler, AE, Ali, AM, Bazarko, A, Chesmore, GE, Coppi, G, Cothard, NF, Dachlythra, N, Devlin, M, Dunner, R, Fabbian, G, Galitzki, N, Golec, JE, Ho, S-PP, Hargrave, PC, Kofman, AM, Lee, AT, Limon, M, Matsuda, FT, Mauskopf, PD, Moodley, K, Nati, F, Niemack, MD, Orlowski-Scherer, J, Page, LA, Partridge, B, Puglisi, G, Reichardt, CL, Sierra, CE, Simon, SM, Teply, GP, Tucker, C, Wollack, EJ, Xu, Z, and Zhu, N
Abstract: We present geometrical and physical optics simulation results for the Simons Observatory Large Aperture Telescope. This work was developed as part of the general design process for the telescope, allowing us to evaluate the impact of various design choices on performance metrics and potential systematic effects. The primary goal of the simulations was to evaluate the final design of the reflectors and the cold optics that are now being built. We describe nonsequential ray tracing used to inform the design of the cold optics, including absorbers internal to each optics tube. We discuss ray tracing simulations of the telescope structure that allow us to determine geometries that minimize detector loading and mitigate spurious near-field effects that have not been resolved by the internal baffling. We also describe physical optics simulations, performed over a range of frequencies and field locations, that produce estimates of monochromatic far-field beam patterns, which in turn are used to gauge general optical performance. Finally, we describe simulations that shed light on beam sidelobes from panel gap diffraction.
Published: 2021

36. The Atacama Cosmology Telescope: Microwave Intensity and Polarization Maps of the Galactic Center

Author: Guan, Y, Guan, Y, Clark, SE, Hensley, BS, Gallardo, PA, Naess, S, Duell, CJ, Aiola, S, Atkins, Z, Calabrese, E, Choi, SK, Cothard, NF, Devlin, M, Duivenvoorden, AJ, Dunkley, J, Dünner, R, Ferraro, S, Hasselfield, M, Hughes, JP, Koopman, BJ, Kosowsky, AB, Madhavacheril, MS, McMahon, J, Nati, F, Niemack, MD, Page, LA, Salatino, M, Schaan, E, Sehgal, N, Sifón, C, Staggs, S, Vavagiakis, EM, Wollack, EJ, Xu, Z, Guan, Y, Guan, Y, Clark, SE, Hensley, BS, Gallardo, PA, Naess, S, Duell, CJ, Aiola, S, Atkins, Z, Calabrese, E, Choi, SK, Cothard, NF, Devlin, M, Duivenvoorden, AJ, Dunkley, J, Dünner, R, Ferraro, S, Hasselfield, M, Hughes, JP, Koopman, BJ, Kosowsky, AB, Madhavacheril, MS, McMahon, J, Nati, F, Niemack, MD, Page, LA, Salatino, M, Schaan, E, Sehgal, N, Sifón, C, Staggs, S, Vavagiakis, EM, Wollack, EJ, and Xu, Z
Abstract: We present arcminute-resolution intensity and polarization maps of the Galactic center made with the Atacama Cosmology Telescope. The maps cover a 32 deg2 field at 98, 150, and 224 GHz with |l| ≤ 4 , |b| ≤ 2 . We combine these data with Planck observations at similar frequencies to create coadded maps with increased sensitivity at large angular scales. With the coadded maps, we are able to resolve many known features of the Central Molecular Zone (CMZ) in both total intensity and polarization. We map the orientation of the plane-of-sky component of the Galactic magnetic field inferred from the polarization angle in the CMZ, finding significant changes in morphology in the three frequency bands as the underlying dominant emission mechanism changes from synchrotron to dust emission. Selected Galactic center sources, including Sgr A∗, the Brick molecular cloud (G0.253+0.016), the Mouse pulsar wind nebula (G359.23-0.82), and the Tornado supernova remnant candidate (G357.7-0.1), are examined in detail. These data illustrate the potential for leveraging ground-based cosmic microwave background polarization experiments for Galactic science.
Published: 2021

37. The Atacama Cosmology Telescope: A Search for Planet 9

Author: Naess, S, Naess, S, Aiola, S, Battaglia, N, Bond, RJ, Calabrese, E, Choi, SK, Cothard, NF, Halpern, M, Hill, JC, Koopman, BJ, Devlin, M, McMahon, J, Dicker, S, Duivenvoorden, AJ, Dunkley, J, Fanfani, V, Ferraro, S, Gallardo, PA, Guan, Y, Han, D, Hasselfield, M, Hincks, AD, Huffenberger, K, Kosowsky, AB, Louis, T, Macinnis, A, Madhavacheril, MS, Nati, F, Niemack, MD, Page, L, Salatino, M, Schaan, E, Orlowski-Scherer, J, Schillaci, A, Schmitt, B, Sehgal, N, Sifón, C, Staggs, S, Engelen, AV, Wollack, EJ, Naess, S, Naess, S, Aiola, S, Battaglia, N, Bond, RJ, Calabrese, E, Choi, SK, Cothard, NF, Halpern, M, Hill, JC, Koopman, BJ, Devlin, M, McMahon, J, Dicker, S, Duivenvoorden, AJ, Dunkley, J, Fanfani, V, Ferraro, S, Gallardo, PA, Guan, Y, Han, D, Hasselfield, M, Hincks, AD, Huffenberger, K, Kosowsky, AB, Louis, T, Macinnis, A, Madhavacheril, MS, Nati, F, Niemack, MD, Page, L, Salatino, M, Schaan, E, Orlowski-Scherer, J, Schillaci, A, Schmitt, B, Sehgal, N, Sifón, C, Staggs, S, Engelen, AV, and Wollack, EJ
Abstract: We use Atacama Cosmology Telescope (ACT) observations at 98 GHz (2015–2019), 150 GHz (2013–2019), and 229 GHz (2017–2019) to perform a blind shift-and-stack search for Planet 9. The search explores distances from 300 au to 2000 au and velocities up to 6.′3 per year, depending on the distance (r). For a 5 Earth-mass Planet 9 the detection limit varies from 325 au to 625 au, depending on the sky location. For a 10 Earth-mass planet the corresponding range is 425 au to 775 au. The predicted aphelion and most likely location of the planet corresponds to the shallower end of these ranges. The search covers the whole 18,000 square degrees of the ACT survey. No significant detections are found, which is used to place limits on the millimeter-wave flux density of Planet 9 over much of its orbit. Overall we eliminate roughly 17% and 9% of the parameter space for a 5 and 10 Earth-mass Planet 9, respectively. These bounds approach those of a recent INPOP19a ephemeris-based analysis, but do not exceed it. We also provide a list of the 10 strongest candidates from the search for possible follow-up. More generally, we exclude (at 95% confidence) the presence of an unknown solar system object within our survey area brighter than 4–12 mJy (depending on position) at 150 GHz with current distance 300 au < r < 600 au and heliocentric angular velocity , corresponding to low-to-moderate eccentricities. These limits worsen gradually beyond 600 au, reaching 5–15 mJy by 1500 au.
Published: 2021

38. The Simons Observatory: metamaterial microwave absorber and its cryogenic applications

Author: Xu, Z, Chesmore, G, Adachi, S, Ali, A, Bazarko, A, Coppi, G, Devlin, M, Devlin, T, Dicker, S, Gallardo, P, Golec, J, Gudmundsson, J, Harrington, K, Hattori, M, Kofman, A, Kiuchi, K, Kusaka, A, Limon, M, Matsuda, F, Mcmahon, J, Nati, F, Niemack, M, Suzuki, A, Teply, G, Thornton, R, Wollack, E, Zannoni, M, Zhu, N, Xu, Zhilei, Chesmore, Grace E., Adachi, Shunsuke, Ali, Aamir M., Bazarko, Andrew, Coppi, Gabriele, Devlin, Mark, Devlin, Tom, Dicker, Simon R., Gallardo, Patricio A., Golec, Joseph E., Gudmundsson, Jon E., Harrington, Kathleen, Hattori, Makoto, Kofman, Anna, Kiuchi, Kenji, Kusaka, Akito, Limon, Michele, Matsuda, Frederick, McMahon, Jeff, Nati, Federico, Niemack, Michael D., Suzuki, Aritoki, Teply, Grant P., Thornton, Robert J., Wollack, Edward J., Zannoni, Mario, Zhu, Ningfeng, Xu, Z, Chesmore, G, Adachi, S, Ali, A, Bazarko, A, Coppi, G, Devlin, M, Devlin, T, Dicker, S, Gallardo, P, Golec, J, Gudmundsson, J, Harrington, K, Hattori, M, Kofman, A, Kiuchi, K, Kusaka, A, Limon, M, Matsuda, F, Mcmahon, J, Nati, F, Niemack, M, Suzuki, A, Teply, G, Thornton, R, Wollack, E, Zannoni, M, Zhu, N, Xu, Zhilei, Chesmore, Grace E., Adachi, Shunsuke, Ali, Aamir M., Bazarko, Andrew, Coppi, Gabriele, Devlin, Mark, Devlin, Tom, Dicker, Simon R., Gallardo, Patricio A., Golec, Joseph E., Gudmundsson, Jon E., Harrington, Kathleen, Hattori, Makoto, Kofman, Anna, Kiuchi, Kenji, Kusaka, Akito, Limon, Michele, Matsuda, Frederick, McMahon, Jeff, Nati, Federico, Niemack, Michael D., Suzuki, Aritoki, Teply, Grant P., Thornton, Robert J., Wollack, Edward J., Zannoni, Mario, and Zhu, Ningfeng
Abstract: Controlling stray light at millimeter wavelengths requires special optical design and selection of absorptive materials that should be compatible with cryogenic operating environments. While a wide selection of absorptive materials exists, these typically exhibit high indices of refraction and reflect/scatter a significant fraction of light before absorption. For many lower index materials such as commercial microwave absorbers, their applications in cryogenic environments are challenging. In this paper, we present a new tool to control stray light: metamaterial microwave absorber tiles. These tiles comprise an outer metamaterial layer that approximates a lossy gradient index anti-reflection coating. They are fabricated via injection molding commercially available carbon-loaded polyurethane (25% by mass). The injection molding technology enables mass production at low cost. The design of these tiles is presented, along with thermal tests to 1 K. Room temperature optical measurements verify their control of reflectance to less than 1% up to 65∘ angles of incidence, and control of wide angle scattering below 0.01%. The dielectric properties of the bulk carbon-loaded material used in the tiles is also measured at different temperatures, confirming that the material maintains similar dielectric properties down to 3 K.
Published: 2021

39. Will #WeThe85 Finally Include #WeThe15 as a Legacy of Tokyo 2020?

Author: Jackson,, D, Bernstein, A, Butterworth, M, Cho, Y, Coombs, DS, Devlin, M, Onwumechili, C, Darcy, S, Dickson, T, Jackson,, D, Bernstein, A, Butterworth, M, Cho, Y, Coombs, DS, Devlin, M, Onwumechili, C, Darcy, S, and Dickson, T
Published: 2021

40. Thermodynamic evolution of the $z=1.75$ galaxy cluster IDCS J1426.5+3508

Author: Andreon, S., Romero, C., Castagna, F., Ragagnin, A., Devlin, M., Dicker, S., Mason, B., Mroczkowski, T., Sarazin, C., Sievers, J., Stanchfield, S., Andreon, S., Romero, C., Castagna, F., Ragagnin, A., Devlin, M., Dicker, S., Mason, B., Mroczkowski, T., Sarazin, C., Sievers, J., and Stanchfield, S.
Abstract: We present resolved thermodynamic profiles out to 500 kpc, about $r_{500}$, of the $z=1.75$ galaxy cluster IDCS J1426.5+3508 with 40 kpc resolution. Thanks to the combination of Sunyaev-Zel'dovich and X-ray datasets, IDCS J1426.5+3508 becomes the most distant cluster with resolved thermodynamic profiles. These are derived assuming a non-parametric pressure profile and a very flexible model for the electron density profile. The shape of the pressure profile is flatter than the universal pressure profile. The IDCS J1426.5+3508 temperature profile is increasing radially out to 500 kpc. To identify the possible future evolution of IDCS J1426.5+3508 , we compared it with its local descendants that numerical simulations show to be $0.65\pm0.12$ dex more massive. We found no evolution at 30 kpc, indicating a fine tuning between cooling and heating at small radii. At $30
Published: 2021
Full Text: View/download PDF

41. The mass and galaxy distribution around SZ-selected clusters

Author: Shin, T., Jain, B., Adhikari, S., Baxter, E. J., Chang, C., Pandey, S., Salcedo, A., Weinberg, D. H., Amsellem, A., Battaglia, N., Belyakov, M., Dacunha, T., Goldstein, S., Kravtsov, A. V., Varga, T. N., Abbott, T. M. C., Aguena, M., Alarcon, A., Allam, S., Amon, A., Andrade-Oliveira, F., Annis, J., Bacon, D., Bechtol, K., Becker, M. R., Bernstein, G. M., Bertin, E., Bocquet, S., Bond, J. R., Brooks, D., Buckley-Geer, E., Burke, D. L., Campos, A., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Chen, R., Choi, A., Costanzi, M., da Costa, L. N., DeRose, J., Desai, S., De Vicente, J., Devlin, M. J., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Doux, C., Drlica-Wagner, A., Eckert, K., Elvin-Poole, J., Everett, S., Ferraro, S., Ferrero, I., Ferté, A., Flaugher, B., Frieman, J., Gallardo, P. A., Gatti, M., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., Harrison, I., Hartley, W. G., Hill, J. C., Hilton, M., Hinton, S. R., Hollowood, D. L., Hughes, J. P., James, D. J., Jarvis, M., Jeltema, T., Koopman, B. J., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Lokken, M., MacCrann, N., Madhavacheril, M. S., Maia, M. A. G., McCullough, J., McMahon, J., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Moodley, K., Morgan, R., Myles, J., Nati, F., Navarro-Alsina, A., Niemack, M. D., Ogando, R. L. C., Page, L. A., Palmese, A., Partridge, B., Paz-Chinchón, F., Pereira, M. E. S., Pieres, A., Malagón, A. A. Plazas, Prat, J., Raveri, M., Rodriguez-Monroy, M., Rollins, R. P., Romer, A. K., Rykoff, E. S., Salatino, M., Sánchez, C., Sanchez, E., Santiago, B., Scarpine, V., Schillaci, A., Secco, L. F., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Sherwin, B. D., Sifón, C., Smith, M., Soares-Santos, M., Staggs, S. T., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Troxel, M. A., Tutusaus, I., Vavagiakis, E. M., Weller, J., Wollack, E. J., Yanny, B., Yin, B., Zhang, Y., Shin, T., Jain, B., Adhikari, S., Baxter, E. J., Chang, C., Pandey, S., Salcedo, A., Weinberg, D. H., Amsellem, A., Battaglia, N., Belyakov, M., Dacunha, T., Goldstein, S., Kravtsov, A. V., Varga, T. N., Abbott, T. M. C., Aguena, M., Alarcon, A., Allam, S., Amon, A., Andrade-Oliveira, F., Annis, J., Bacon, D., Bechtol, K., Becker, M. R., Bernstein, G. M., Bertin, E., Bocquet, S., Bond, J. R., Brooks, D., Buckley-Geer, E., Burke, D. L., Campos, A., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Chen, R., Choi, A., Costanzi, M., da Costa, L. N., DeRose, J., Desai, S., De Vicente, J., Devlin, M. J., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Doux, C., Drlica-Wagner, A., Eckert, K., Elvin-Poole, J., Everett, S., Ferraro, S., Ferrero, I., Ferté, A., Flaugher, B., Frieman, J., Gallardo, P. A., Gatti, M., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., Harrison, I., Hartley, W. G., Hill, J. C., Hilton, M., Hinton, S. R., Hollowood, D. L., Hughes, J. P., James, D. J., Jarvis, M., Jeltema, T., Koopman, B. J., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Lokken, M., MacCrann, N., Madhavacheril, M. S., Maia, M. A. G., McCullough, J., McMahon, J., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Moodley, K., Morgan, R., Myles, J., Nati, F., Navarro-Alsina, A., Niemack, M. D., Ogando, R. L. C., Page, L. A., Palmese, A., Partridge, B., Paz-Chinchón, F., Pereira, M. E. S., Pieres, A., Malagón, A. A. Plazas, Prat, J., Raveri, M., Rodriguez-Monroy, M., Rollins, R. P., Romer, A. K., Rykoff, E. S., Salatino, M., Sánchez, C., Sanchez, E., Santiago, B., Scarpine, V., Schillaci, A., Secco, L. F., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Sherwin, B. D., Sifón, C., Smith, M., Soares-Santos, M., Staggs, S. T., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Troxel, M. A., Tutusaus, I., Vavagiakis, E. M., Weller, J., Wollack, E. J., Yanny, B., Yin, B., and Zhang, Y.
Abstract: We present measurements of the radial profiles of the mass and galaxy number density around Sunyaev-Zel'dovich-selected clusters using both weak lensing and galaxy counts. The clusters are selected from the Atacama Cosmology Telescope Data Release 5 and the galaxies from the Dark Energy Survey Year 3 dataset. With signal-to-noise of 62 (43) for galaxy (weak lensing) profiles over scales of about $0.2-20h^{-1}$ Mpc, these are the highest precision measurements for SZ-selected clusters to date. Because SZ selection closely approximates mass selection, these measurements enable several tests of theoretical models of the mass and light distribution around clusters. Our main findings are: 1. The splashback feature is detected at a consistent location in both the mass and galaxy profiles and its location is consistent with predictions of cold dark matter N-body simulations. 2. The full mass profile is also consistent with the simulations; hence it can constrain alternative dark matter models that modify the mass distribution of clusters. 3. The shapes of the galaxy and lensing profiles are remarkably similar for our sample over the entire range of scales, from well inside the cluster halo to the quasilinear regime. This can be used to constrain processes such as quenching and tidal disruption that alter the galaxy distribution inside the halo, and scale-dependent features in the transition regime outside the halo. We measure the dependence of the profile shapes on the galaxy sample, redshift and cluster mass. We extend the Diemer \& Kravtsov model for the cluster profiles to the linear regime using perturbation theory and show that it provides a good match to the measured profiles. We also compare the measured profiles to predictions of the standard halo model and simulations that include hydrodynamics. Applications of these results to cluster mass estimation and cosmology are discussed., Comment: 15 pages, 6 figures (main) + 3 pages, 6 figures (appendix), submitted to MNRAS
Published: 2021
Full Text: View/download PDF

42. The Atacama Cosmology Telescope: A Search for Planet 9

Author: Naess, S, Aiola, S, Battaglia, N, Bond, R, Calabrese, E, Choi, S, Cothard, N, Halpern, M, Colin Hill, J, Koopman, B, Devlin, M, Mcmahon, J, Dicker, S, Duivenvoorden, A, Dunkley, J, Fanfani, V, Ferraro, S, Gallardo, P, Guan, Y, Han, D, Hasselfield, M, Hincks, A, Huffenberger, K, Kosowsky, A, Louis, T, Macinnis, A, Madhavacheril, M, Nati, F, Niemack, M, Page, L, Salatino, M, Schaan, E, Orlowski-Scherer, J, Schillaci, A, Schmitt, B, Sehgal, N, Sif??n, C, Staggs, S, Van Engelen, A, Wollack, E, Sigurd Naess, Simone Aiola, Nick Battaglia, Richard J. Bond, Erminia Calabrese, Steve K. Choi, Nicholas F. Cothard, Mark Halpern, J. Colin Hill, Brian J. Koopman, Mark Devlin, Jeff McMahon, Simon Dicker, Adriaan J. Duivenvoorden, Jo Dunkley, Valentina Fanfani, Simone Ferraro, Patricio A. Gallardo, Yilun Guan, Dongwon Han, Matthew Hasselfield, Adam D. Hincks, Kevin Huffenberger, Arthur B. Kosowsky, Thibaut Louis, Amanda Macinnis, Mathew S. Madhavacheril, Federico Nati, Michael D. Niemack, Lyman Page, Maria Salatino, Emmanuel Schaan, John Orlowski-Scherer, Alessandro Schillaci, Benjamin Schmitt, Neelima Sehgal, Crist??bal Sif??n, Suzanne Staggs, Alexander Van Engelen, Edward J. Wollack, Naess, S, Aiola, S, Battaglia, N, Bond, R, Calabrese, E, Choi, S, Cothard, N, Halpern, M, Colin Hill, J, Koopman, B, Devlin, M, Mcmahon, J, Dicker, S, Duivenvoorden, A, Dunkley, J, Fanfani, V, Ferraro, S, Gallardo, P, Guan, Y, Han, D, Hasselfield, M, Hincks, A, Huffenberger, K, Kosowsky, A, Louis, T, Macinnis, A, Madhavacheril, M, Nati, F, Niemack, M, Page, L, Salatino, M, Schaan, E, Orlowski-Scherer, J, Schillaci, A, Schmitt, B, Sehgal, N, Sif??n, C, Staggs, S, Van Engelen, A, Wollack, E, Sigurd Naess, Simone Aiola, Nick Battaglia, Richard J. Bond, Erminia Calabrese, Steve K. Choi, Nicholas F. Cothard, Mark Halpern, J. Colin Hill, Brian J. Koopman, Mark Devlin, Jeff McMahon, Simon Dicker, Adriaan J. Duivenvoorden, Jo Dunkley, Valentina Fanfani, Simone Ferraro, Patricio A. Gallardo, Yilun Guan, Dongwon Han, Matthew Hasselfield, Adam D. Hincks, Kevin Huffenberger, Arthur B. Kosowsky, Thibaut Louis, Amanda Macinnis, Mathew S. Madhavacheril, Federico Nati, Michael D. Niemack, Lyman Page, Maria Salatino, Emmanuel Schaan, John Orlowski-Scherer, Alessandro Schillaci, Benjamin Schmitt, Neelima Sehgal, Crist??bal Sif??n, Suzanne Staggs, Alexander Van Engelen, and Edward J. Wollack
Abstract: We use Atacama Cosmology Telescope (ACT) observations at 98 GHz (2015-2019), 150 GHz (2013-2019), and 229 GHz (2017-2019) to perform a blind shift-and-stack search for Planet 9. The search explores distances from 300 au to 2000 au and velocities up to 6.'3 per year, depending on the distance (r). For a 5 Earth-mass Planet 9 the detection limit varies from 325 au to 625 au, depending on the sky location. For a 10 Earth-mass planet the corresponding range is 425 au to 775 au. The predicted aphelion and most likely location of the planet corresponds to the shallower end of these ranges. The search covers the whole 18,000 square degrees of the ACT survey. No significant detections are found, which is used to place limits on the millimeter-wave flux density of Planet 9 over much of its orbit. Overall we eliminate roughly 17% and 9% of the parameter space for a 5 and 10 Earth-mass Planet 9, respectively. These bounds approach those of a recent INPOP19a ephemeris-based analysis, but do not exceed it. We also provide a list of the 10 strongest candidates from the search for possible follow-up. More generally, we exclude (at 95% confidence) the presence of an unknown solar system object within our survey area brighter than 4-12 mJy (depending on position) at 150 GHz with current distance 300 au < r < 600 au and heliocentric angular velocity 1.'5 yr(-1) < nu.500 au/r< 2.'' 3 yr(-1), corresponding to low-to-moderate eccentricities. These limits worsen gradually beyond 600 au, reaching 5-15 mJy by 1500 au.
Published: 2021

43. The Simons Observatory Large Aperture Telescope Receiver

Author: Zhu, N, Bhandarkar, T, Coppi, G, Kofman, A, Orlowski-Scherer, J, Xu, Z, Adachi, S, Ade, P, Aiola, S, Austermann, J, Bazarko, A, Beall, J, Bhimani, S, Richard Bond, J, Chesmore, G, Choi, S, Connors, J, Cothard, N, Devlin, M, Dicker, S, Dober, B, Duell, C, Duff, S, Dünner, R, Fabbian, G, Galitzki, N, Gallardo, P, Golec, J, Haridas, S, Harrington, K, Healy, E, Patty Ho, S, Huber, Z, Hubmayr, J, Iuliano, J, Johnson, B, Keatin, B, Kiuchi, K, Koopman, B, Lashner, J, Lee, A, Li, Y, Limon, M, Link, M, J Lucas, T, Mccarrick, H, Moore, J, Nati, F, Newburgh, L, Niemack, M, Pierpaoli, E, Randall, M, Perez Sarmiento, K, Saunders, L, Seibert, J, Sierra, C, Sonka, R, Spisak, J, Sutariya, S, Tajima, O, Teply, G, Thornton, R, Tsan, T, Tucker, C, Ullom, J, Vavagiakis, E, Vissers, M, Walker, S, Westbrook, B, Wollack, E, Zannoni, M, Ningfeng Zhu, Tanay Bhandarkar, Gabriele Coppi, Anna M. Kofman, John L. Orlowski-Scherer, Zhilei Xu, Shunsuke Adachi, Peter Ade, Simone Aiola, Jason Austermann, Andrew O. Bazarko, James A. Beall, Sanah Bhimani, J. Richard Bond, Grace E. Chesmore, Steve K. Choi, Jake Connors, Nicholas F. Cothard, Mark Devlin, Simon Dicker, Bradley Dober, Cody J. Duell, Shannon M. Duff, Rolando Dünner, Giulio Fabbian, Nicholas Galitzki, Patricio A. Gallardo, Joseph E. Golec, Saianeesh K. Haridas, Kathleen Harrington, Erin Healy, Shuay-Pwu Patty Ho, Zachary B. Huber, Johannes Hubmayr, Jeffrey Iuliano, Bradley R. Johnson, Brian Keatin, Kenji Kiuchi, Brian J. Koopman, Jack Lashner, Adrian T. Lee, Yaqiong Li, Michele Limon, Michael Link, Tammy J Lucas, Heather McCarrick, Jenna Moore, Federico Nati, Laura B. Newburgh, Michael D. Niemack, Elena Pierpaoli, Michael J. Randall, Karen Perez Sarmiento, Lauren J. Saunders, Joseph Seibert, Carlos Sierra, Rita Sonka, Jacob Spisak, Shreya Sutariya, Osamu Tajima, Grant P. Teply, Robert J. Thornton, Tran Tsan, Carole Tucker, Joel Ullom, Eve M. Vavagiakis, Michael R. Vissers, Samantha Walker, Benjamin Westbrook, Edward J. Wollack, Mario Zannoni, Zhu, N, Bhandarkar, T, Coppi, G, Kofman, A, Orlowski-Scherer, J, Xu, Z, Adachi, S, Ade, P, Aiola, S, Austermann, J, Bazarko, A, Beall, J, Bhimani, S, Richard Bond, J, Chesmore, G, Choi, S, Connors, J, Cothard, N, Devlin, M, Dicker, S, Dober, B, Duell, C, Duff, S, Dünner, R, Fabbian, G, Galitzki, N, Gallardo, P, Golec, J, Haridas, S, Harrington, K, Healy, E, Patty Ho, S, Huber, Z, Hubmayr, J, Iuliano, J, Johnson, B, Keatin, B, Kiuchi, K, Koopman, B, Lashner, J, Lee, A, Li, Y, Limon, M, Link, M, J Lucas, T, Mccarrick, H, Moore, J, Nati, F, Newburgh, L, Niemack, M, Pierpaoli, E, Randall, M, Perez Sarmiento, K, Saunders, L, Seibert, J, Sierra, C, Sonka, R, Spisak, J, Sutariya, S, Tajima, O, Teply, G, Thornton, R, Tsan, T, Tucker, C, Ullom, J, Vavagiakis, E, Vissers, M, Walker, S, Westbrook, B, Wollack, E, Zannoni, M, Ningfeng Zhu, Tanay Bhandarkar, Gabriele Coppi, Anna M. Kofman, John L. Orlowski-Scherer, Zhilei Xu, Shunsuke Adachi, Peter Ade, Simone Aiola, Jason Austermann, Andrew O. Bazarko, James A. Beall, Sanah Bhimani, J. Richard Bond, Grace E. Chesmore, Steve K. Choi, Jake Connors, Nicholas F. Cothard, Mark Devlin, Simon Dicker, Bradley Dober, Cody J. Duell, Shannon M. Duff, Rolando Dünner, Giulio Fabbian, Nicholas Galitzki, Patricio A. Gallardo, Joseph E. Golec, Saianeesh K. Haridas, Kathleen Harrington, Erin Healy, Shuay-Pwu Patty Ho, Zachary B. Huber, Johannes Hubmayr, Jeffrey Iuliano, Bradley R. Johnson, Brian Keatin, Kenji Kiuchi, Brian J. Koopman, Jack Lashner, Adrian T. Lee, Yaqiong Li, Michele Limon, Michael Link, Tammy J Lucas, Heather McCarrick, Jenna Moore, Federico Nati, Laura B. Newburgh, Michael D. Niemack, Elena Pierpaoli, Michael J. Randall, Karen Perez Sarmiento, Lauren J. Saunders, Joseph Seibert, Carlos Sierra, Rita Sonka, Jacob Spisak, Shreya Sutariya, Osamu Tajima, Grant P. Teply, Robert J. Thornton, Tran Tsan, Carole Tucker, Joel Ullom, Eve M. Vavagiakis, Michael R. Vissers, Samantha Walker, Benjamin Westbrook, Edward J. Wollack, and Mario Zannoni
Abstract: The Simons Observatory is a ground-based cosmic microwave background experiment that consists of three 0.4 m small-aperture telescopes and one 6 m Large Aperture Telescope, located at an elevation of 5300 m on Cerro Toco in Chile. The Simons Observatory Large Aperture Telescope Receiver (LATR) is the cryogenic camera that will be coupled to the Large Aperture Telescope. The resulting instrument will produce arcminute-resolution millimeter-wave maps of half the sky with unprecedented precision. The LATR is the largest cryogenic millimeter-wave camera built to date, with a diameter of 2.4 m and a length of 2.6 m. The coldest stage of the camera is cooled to 100 mK, the operating temperature of the bolometric detectors with bands centered around 27, 39, 93, 145, 225, and 280 GHz. Ultimately, the LATR will accommodate 13 40 cm diameter optics tubes, each with three detector wafers and a total of 62,000 detectors. The LATR design must simultaneously maintain the optical alignment of the system, control stray light, provide cryogenic isolation, limit thermal gradients, and minimize the time to cool the system from room temperature to 100 mK. The interplay between these competing factors poses unique challenges. We discuss the trade studies involved with the design, the final optimization, the construction, and ultimate performance of the system.
Published: 2021

44. The Simons Observatory: modeling optical systematics in the Large Aperture Telescope

Author: Gudmundsson, J, Gallardo, P, Puddu, R, Dicker, S, Adler, A, Ali, A, Bazarko, A, Chesmore, G, Coppi, G, Cothard, N, Dachlythra, N, Devlin, M, Dünner, R, Fabbian, G, Galitzki, N, Golec, J, Patty Ho, S, Hargrave, P, Kofman, A, Lee, A, Limon, M, Matsuda, F, Mauskopf, P, Moodley, K, Nati, F, Niemack, M, Orlowski-Scherer, J, Page, L, Partridge, B, Puglisi, G, Reichardt, C, Sierra, C, Simon, S, Teply, G, Tucker, C, Wollack, E, Xu, Z, Zhu, N, Gudmundsson, Jon E., Gallardo, Patricio A., Puddu, Roberto, Dicker, Simon R., Adler, Alexandre E., Ali, Aamir M., Bazarko, Andrew, Chesmore, Grace E., Coppi, Gabriele, Cothard, Nicholas F., Dachlythra, Nadia, Devlin, Mark, Dünner, Rolando, Fabbian, Giulio, Galitzki, Nicholas, Golec, Joseph E., Patty Ho, Shuay-Pwu, Hargrave, Peter C., Kofman, Anna M., Lee, Adrian T., Limon, Michele, Matsuda, Frederick T., Mauskopf, Philip D., Moodley, Kavilan, Nati, Federico, Niemack, Michael D., Orlowski-Scherer, John, Page, Lyman A., Partridge, Bruce, Puglisi, Giuseppe, Reichardt, Christian L., Sierra, Carlos E., Simon, Sara M., Teply, Grant P., Tucker, Carole, Wollack, Edward J., Xu, Zhilei, Zhu, Ningfeng, Gudmundsson, J, Gallardo, P, Puddu, R, Dicker, S, Adler, A, Ali, A, Bazarko, A, Chesmore, G, Coppi, G, Cothard, N, Dachlythra, N, Devlin, M, Dünner, R, Fabbian, G, Galitzki, N, Golec, J, Patty Ho, S, Hargrave, P, Kofman, A, Lee, A, Limon, M, Matsuda, F, Mauskopf, P, Moodley, K, Nati, F, Niemack, M, Orlowski-Scherer, J, Page, L, Partridge, B, Puglisi, G, Reichardt, C, Sierra, C, Simon, S, Teply, G, Tucker, C, Wollack, E, Xu, Z, Zhu, N, Gudmundsson, Jon E., Gallardo, Patricio A., Puddu, Roberto, Dicker, Simon R., Adler, Alexandre E., Ali, Aamir M., Bazarko, Andrew, Chesmore, Grace E., Coppi, Gabriele, Cothard, Nicholas F., Dachlythra, Nadia, Devlin, Mark, Dünner, Rolando, Fabbian, Giulio, Galitzki, Nicholas, Golec, Joseph E., Patty Ho, Shuay-Pwu, Hargrave, Peter C., Kofman, Anna M., Lee, Adrian T., Limon, Michele, Matsuda, Frederick T., Mauskopf, Philip D., Moodley, Kavilan, Nati, Federico, Niemack, Michael D., Orlowski-Scherer, John, Page, Lyman A., Partridge, Bruce, Puglisi, Giuseppe, Reichardt, Christian L., Sierra, Carlos E., Simon, Sara M., Teply, Grant P., Tucker, Carole, Wollack, Edward J., Xu, Zhilei, and Zhu, Ningfeng
Abstract: We present geometrical and physical optics simulation results for the Simons Observatory Large Aperture Telescope. This work was developed as part of the general design process for the telescope, allowing us to evaluate the impact of various design choices on performance metrics and potential systematic effects. The primary goal of the simulations was to evaluate the final design of the reflectors and the cold optics that are now being built. We describe nonsequential ray tracing used to inform the design of the cold optics, including absorbers internal to each optics tube. We discuss ray tracing simulations of the telescope structure that allow us to determine geometries that minimize detector loading and mitigate spurious near-field effects that have not been resolved by the internal baffling. We also describe physical optics simulations, performed over a range of frequencies and field locations, that produce estimates of monochromatic far-field beam patterns, which in turn are used to gauge general optical performance. Finally, we describe simulations that shed light on beam sidelobes from panel gap diffraction.
Published: 2021

45. Acoustic Communication and Sensing for Inflatable Modular Soft Robots

Author: Drew, D. S., Devlin, M., Hawkes, E., Follmer, S., Drew, D. S., Devlin, M., Hawkes, E., and Follmer, S.
Abstract: Modular soft robots combine the strengths of two traditionally separate areas of robotics. As modular robots, they can show robustness to individual failure and reconfigurability; as soft robots, they can deform and undergo large shape changes in order to adapt to their environment, and have inherent human safety. However, for sensing and communication these robots also combine the challenges of both: they require solutions that are scalable (low cost and complexity) and efficient (low power) to enable collectives of large numbers of robots, and these solutions must also be able to interface with the high extension ratio elastic bodies of soft robots. In this work, we seek to address these challenges using acoustic signals produced by piezoelectric surface transducers that are cheap, simple, and low power, and that not only integrate with but also leverage the elastic robot skins for signal transmission. Importantly, to further increase scalability, the transducers exhibit multi-functionality made possible by a relatively flat frequency response across the audible and ultrasonic ranges. With minimal hardware, they enable directional contact-based communication, audible-range communication at a distance, and exteroceptive sensing. We demonstrate a subset of the decentralized collective behaviors these functions make possible with multi-robot hardware implementations. The use of acoustic waves in this domain is shown to provide distinct advantages over existing solutions., Comment: 7 pages, 9 figures, conference
Published: 2021

46. Reshaping the Superhuman to the Super Ordinary: Observations on the Tokyo 2021 Paralympic Games

Author: Jackson, D, Bernstein, A, Butterworth, M, Cho, Y, Coombs, DS, Devlin, M, Onwumechili, C, Darcy, S, Dickson, T, Jackson, D, Bernstein, A, Butterworth, M, Cho, Y, Coombs, DS, Devlin, M, Onwumechili, C, Darcy, S, and Dickson, T
Published: 2021

47. Will #WeThe85 Finally Include #WeThe15 as a Legacy of Tokyo 2020?

Author: Jackson,, D, Bernstein, A, Butterworth, M, Cho, Y, Coombs, DS, Devlin, M, Onwumechili, C, Darcy, S, Dickson, T, Jackson,, D, Bernstein, A, Butterworth, M, Cho, Y, Coombs, DS, Devlin, M, Onwumechili, C, Darcy, S, and Dickson, T
Published: 2021

48. Reshaping the Superhuman to the Super Ordinary: Observations on the Tokyo 2021 Paralympic Games

Author: Jackson, D, Bernstein, A, Butterworth, M, Cho, Y, Coombs, DS, Devlin, M, Onwumechili, C, Darcy, S, Dickson, T, Jackson, D, Bernstein, A, Butterworth, M, Cho, Y, Coombs, DS, Devlin, M, Onwumechili, C, Darcy, S, and Dickson, T
Published: 2021

49. Non-Gaussianity of secondary anisotropies from ACTPol and Planck

Author: Coulton, W, Aiola, S, Battaglia, N, Calabrese, E, Choi, S, Devlin, M, Gallardo, P, Hill, J, Hincks, A, Hubmayr, J, Hughes, J, Kosowsky, A, Louis, T, Madhavacheril, M, Loic, M, Naess, S, Nati, F, Niemack, M, Page, L, Partridge, B, Sherwin, B, Spergel, D, Staggs, S, Engelen, A, Wollack, E, Coulton W. R., Aiola S., Battaglia N., Calabrese E., Choi S. K., Devlin M. J., Gallardo P. A., Hill J. C., Hincks A. D., Hubmayr J., Hughes J. P., Kosowsky A., Louis T., Madhavacheril M. S., Loic M., Naess S., Nati F., Niemack M. D., Page L. A., Partridge B., Sherwin B. D., Spergel D. N., Staggs S. T., Engelen A. V., Wollack E. J., Coulton, W, Aiola, S, Battaglia, N, Calabrese, E, Choi, S, Devlin, M, Gallardo, P, Hill, J, Hincks, A, Hubmayr, J, Hughes, J, Kosowsky, A, Louis, T, Madhavacheril, M, Loic, M, Naess, S, Nati, F, Niemack, M, Page, L, Partridge, B, Sherwin, B, Spergel, D, Staggs, S, Engelen, A, Wollack, E, Coulton W. R., Aiola S., Battaglia N., Calabrese E., Choi S. K., Devlin M. J., Gallardo P. A., Hill J. C., Hincks A. D., Hubmayr J., Hughes J. P., Kosowsky A., Louis T., Madhavacheril M. S., Loic M., Naess S., Nati F., Niemack M. D., Page L. A., Partridge B., Sherwin B. D., Spergel D. N., Staggs S. T., Engelen A. V., and Wollack E. J.
Abstract: Most secondary sources of cosmic microwave background anisotropy (radio sources, dusty galaxies, thermal Sunyaev Zel'dovich distortions from hot gas, and gravitational lensing) are highly non-Gaussian. Statistics beyond the power spectrum are therefore potentially important sources of information about the physics of these processes. We combine data from the Atacama Cosmology Telescope and with data from the Planck satellite (only using Planck data in the overlapping region) to constrain the amplitudes of a set of theoretical bispectrum templates from the thermal Sunyaev-Zeldovich (tSZ) effect, dusty star-forming galaxies (DSFGs), gravitational lensing, and radio galaxies. We make a strong detection of radio galaxies (> 5 sigma) and have hints of non-Gaussianity arising from the tSZ effect, DSFGs, from cross-correlations between the tSZ effect and DSFGs and from cross-correlations among the tSZ effect, DSFGs and radio galaxies. These results suggest that the same halos host radio sources, DSFGs, and have tSZ signal. We present a new method to calculate the non-Gaussian contributions to the template covariances. Using this method we find significant non-Gaussian contributions to the variance and covariance of our templates, with templates involving the tSZ effect most effected. Strong degeneracies exist between the various sources at the current noise levels. In light of these degeneracies, combined with theoretical uncertainty in the templates, these results are a demonstration of this technique. With these caveats, we demonstrate the utility of future bispectrum measurements by using the tSZ bispectrum measurement to constrain a combination of the amplitude of matter fluctuations and the matter density to be sigma(8)Omega(0.17)(m) = 0.65(-0.06)(+0.05). Improvements in signal to noise from upcoming Advanced ACT, SPT-3G, Simons Observatory, and CMB-S4 observations will enable the separation of bispectrum components and robust constraints on cosmological parameters
Published: 2018

50. Simons Observatory large aperture receiver simulation overview

Author: Orlowski-Scherer, J, Zhu, N, Xu, Z, Ali, A, Arnold, K, Ashton, P, Coppi, G, Devlin, M, Dicker, S, Galitzki, N, Gallardo, P, Keating, B, Lee, A, Limon, M, Lungu, M, May, A, Mcmahon, J, Niemack, M, Piccirillo, L, Puglisi, G, Salatino, M, Silva-Feaver, M, Simon, S, Thornton, R, Vavagiakis, E, Orlowski-Scherer J. L., Zhu N., Xu Z., Ali A., Arnold K. S., Ashton P. C., Coppi G., Devlin M., Dicker S., Galitzki N., Gallardo P. A., Keating B., Lee A. T., Limon M., Lungu M., May A., McMahon J., Niemack M. D., Piccirillo L., Puglisi G., Salatino M., Silva-Feaver M., Simon S. M., Thornton R., Vavagiakis E. M., Orlowski-Scherer, J, Zhu, N, Xu, Z, Ali, A, Arnold, K, Ashton, P, Coppi, G, Devlin, M, Dicker, S, Galitzki, N, Gallardo, P, Keating, B, Lee, A, Limon, M, Lungu, M, May, A, Mcmahon, J, Niemack, M, Piccirillo, L, Puglisi, G, Salatino, M, Silva-Feaver, M, Simon, S, Thornton, R, Vavagiakis, E, Orlowski-Scherer J. L., Zhu N., Xu Z., Ali A., Arnold K. S., Ashton P. C., Coppi G., Devlin M., Dicker S., Galitzki N., Gallardo P. A., Keating B., Lee A. T., Limon M., Lungu M., May A., McMahon J., Niemack M. D., Piccirillo L., Puglisi G., Salatino M., Silva-Feaver M., Simon S. M., Thornton R., and Vavagiakis E. M.
Abstract: The Simons Observatory (SO) will make precision temperature and polarization measurements of the cosmic microwave background (CMB) using a series of telescopes which will cover angular scales between one arcminute and tens of degrees, contain over 60,000 detectors, and sample frequencies between 27 and 270 GHz. SO will consist of a six-meter-aperture telescope coupled to over 30,000 detectors along with an array of half-meter aperture refractive cameras, which together couple to an additional 30,000+ detectors. SO will measure fundamental cosmological parameters of our universe, find high redshift clusters via the Sunyaev-Zeldovich effect, constrain properties of neutrinos, and seek signatures of dark matter through gravitational lensing. In this paper we will present results of the simulations of the SO large aperture telescope receiver (LATR). We will show details of simulations performed to ensure the structural integrity and thermal performance of our receiver, as well as will present the results of finite element analyses (FEA) of designs for the structural support system. Additionally, a full thermal model for the LATR will be described. The model will be used to ensure we meet our design requirements. Finally, we will present the results of FEA used to identify the primary vibrational modes, and planned methods for suppressing these modes. Design solutions to each of these problems that have been informed by simulation will be presented.
Published: 2018

Catalog

Books, media, physical & digital resources

See catalog results

Searchworks

Select search scope, currently: Articles Catalog books, media & more in Jio Institute collections Articles journal articles & other e-resources

Search

Search Constraints

Refine your results

Search Limiters

Publication Year Range

Publication Type

Database

Publisher

343 results on '"Devlin, M"'

Search Results

Catalog

Select search scope, currently: Articles

Catalog

books, media & more in Jio Institute collections

Articles

journal articles & other e-resources