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Start Over Author "Bianchini F" Journal monthly notices of the royal astronomical society
5 results on '"Bianchini F"'

1. Fractional Polarisation of Extragalactic Sources in the 500-square-degree SPTpol Survey

Author

Gupta, N, Reichardt, CL, Ade, PAR, Anderson, AJ, Archipley, M, Austermann, JE, Avva, JS, Beall, JA, Bender, AN, Benson, BA, Bianchini, F, Bleem, LE, Carlstrom, JE, Chang, CL, Chiang, HC, Citron, R, Moran, C Corbett, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, W, Feng, C, Gallicchio, J, George, EM, Gilbert, A, Halverson, NW, Harrington, N, Henning, JW, Hilton, GC, Holder, GP, Holzapfel, WL, Hou, Z, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Knox, L, Lee, AT, Li, D, Lowitz, A, Luong-Van, D, Marrone, DP, McMahon, JJ, Meyer, SS, Mocanu, LM, Mohr, JJ, Montgomery, J, Nadolski, A, Natoli, T, Nibarger, JP, Noble, GI, Novosad, V, Padin, S, Patil, S, Pryke, C, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Shirokoff, E, Sievers, C, Smecher, G, Staniszewski, Z, Stark, AA, Story, KT, Switzer, ER, Tucker, C, Vanderlinde, K, Veach, T, Vieira, JD, Wang, G, Whitehorn, N, Williamson, R, Wu, WLK, Yefremenko, V, and Zhang, L

Subjects
Astronomical Sciences, Physical Sciences, polarization, galaxies: active, cosmology: observations, astro-ph.CO, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

We study the polarization properties of extragalactic sources at 95 and 150 GHz in the SPTpol 500 deg2 survey. We estimate the polarized power by stacking maps at known source positions, and correct for noise bias by subtracting the mean polarized power at random positions in the maps. We show that the method is unbiased using a set of simulated maps with similar noise properties to the real SPTpol maps. We find a flux-weighted mean-squared polarization fraction 〈p2〉= [8.9 ± 1.1] × 10−4 at 95 GHz and [6.9 ± 1.1] × 10−4 at 150 GHz for the full sample. This is consistent with the values obtained for a subsample of active galactic nuclei. For dusty sources, we find 95 per cent upper limits of 〈p2〉95 < 16.9 × 10−3 and 〈p2〉150 < 2.6 × 10−3. We find no evidence that the polarization fraction depends on the source flux or observing frequency. The 1σ upper limit on measured mean-squared polarization fraction at 150 GHz implies that extragalactic foregrounds will be subdominant to the CMB E and B mode polarization power spectra out to at least ℓ ≲ 5700 (ℓ ≲ 4700) and ℓ ≲ 5300 (ℓ ≲ 3600), respectively, at 95 (150) GHz.

Published
2019

2. Fractional polarization of extragalactic sources in the 500 deg2 SPTpol survey

Author

Gupta, N, Reichardt, CL, Ade, PAR, Anderson, AJ, Archipley, M, Austermann, JE, Avva, JS, Beall, JA, Bender, AN, Benson, BA, Bianchini, F, Bleem, LE, Carlstrom, JE, Chang, CL, Chiang, HC, Citron, R, Corbett Moran, C, Crawford, TM, Crites, AT, de Haan, T, Dobbs, MA, Everett, W, Feng, C, Gallicchio, J, George, EM, Gilbert, A, Halverson, NW, Harrington, N, Henning, JW, Hilton, GC, Holder, GP, Holzapfel, WL, Hou, Z, Hrubes, JD, Huang, N, Hubmayr, J, Irwin, KD, Knox, L, Lee, AT, Li, D, Lowitz, A, Luong-Van, D, Marrone, DP, McMahon, JJ, Meyer, SS, Mocanu, LM, Mohr, JJ, Montgomery, J, Nadolski, A, Natoli, T, Nibarger, JP, Noble, GI, Novosad, V, Padin, S, Patil, S, Pryke, C, Ruhl, JE, Saliwanchik, BR, Sayre, JT, Schaffer, KK, Shirokoff, E, Sievers, C, Smecher, G, Staniszewski, Z, Stark, AA, Story, KT, Switzer, ER, Tucker, C, Vanderlinde, K, Veach, T, Vieira, JD, Wang, G, Whitehorn, N, Williamson, R, Wu, WLK, Yefremenko, V, and Zhang, L

Subjects
polarization, galaxies: active, cosmology: observations, astro-ph.CO, Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract

We study the polarization properties of extragalactic sources at 95 and 150 GHz in the SPTpol 500 deg2 survey. We estimate the polarized power by stacking maps at known source positions, and correct for noise bias by subtracting the mean polarized power at random positions in the maps. We show that the method is unbiased using a set of simulated maps with similar noise properties to the real SPTpol maps. We find a flux-weighted mean-squared polarization fraction 〈p2〉= [8.9 ± 1.1] × 10−4 at 95 GHz and [6.9 ± 1.1] × 10−4 at 150 GHz for the full sample. This is consistent with the values obtained for a subsample of active galactic nuclei. For dusty sources, we find 95 per cent upper limits of 〈p2〉95 < 16.9 × 10−3 and 〈p2〉150 < 2.6 × 10−3. We find no evidence that the polarization fraction depends on the source flux or observing frequency. The 1σ upper limit on measured mean-squared polarization fraction at 150 GHz implies that extragalactic foregrounds will be subdominant to the CMB E and B mode polarization power spectra out to at least ℓ ≲ 5700 (ℓ ≲ 4700) and ℓ ≲ 5300 (ℓ ≲ 3600), respectively, at 95 (150) GHz.

Published
2019

3. Constraining radio mode feedback in galaxy clusters with the cluster radio AGNs properties to z ∼ 1

Author

Gupta, N, primary, Pannella, M, additional, Mohr, J J, additional, Klein, M, additional, Rykoff, E S, additional, Annis, J, additional, Avila, S, additional, Bianchini, F, additional, Brooks, D, additional, Buckley-Geer, E, additional, Bulbul, E, additional, Carnero Rosell, A, additional, Carrasco Kind, M, additional, Carretero, J, additional, Chiu, I, additional, Costanzi, M, additional, da Costa, L N, additional, De Vicente, J, additional, Desai, S, additional, Dietrich, J P, additional, Doel, P, additional, Everett, S, additional, Evrard, A E, additional, García-Bellido, J, additional, Gaztanaga, E, additional, Gruen, D, additional, Gruendl, R A, additional, Gschwend, J, additional, Gutierrez, G, additional, Hollowood, D L, additional, Honscheid, K, additional, James, D J, additional, Jeltema, T, additional, Kuehn, K, additional, Lidman, C, additional, Lima, M, additional, Maia, M A G, additional, Marshall, J L, additional, McDonald, M, additional, Menanteau, F, additional, Miquel, R, additional, Ogando, R L C, additional, Palmese, A, additional, Paz-Chinchón, F, additional, Plazas, A A, additional, Reichardt, C L, additional, Sanchez, E, additional, Santiago, B, additional, Saro, A, additional, Scarpine, V, additional, Schindler, R, additional, Schubnell, M, additional, Serrano, S, additional, Sevilla-Noarbe, I, additional, Shao, X, additional, Smith, M, additional, Stott, J P, additional, Strazzullo, V, additional, Suchyta, E, additional, Swanson, M E C, additional, Vikram, V, additional, and Zenteno, A, additional

Published
2020
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4. Fractional polarization of extragalactic sources in the 500 deg2 SPTpol survey.

Author

Gupta, N, Reichardt, C L, Ade, P A R, Anderson, A J, Archipley, M, Austermann, J E, Avva, J S, Beall, J A, Bender, A N, Benson, B A, Bianchini, F, Bleem, L E, Carlstrom, J E, Chang, C L, Chiang, H C, Citron, R, Moran, C Corbett, Crawford, T M, Crites, A T, and de Haan, T

Subjects
ACTIVE galactic nuclei, ARITHMETIC mean, POWER spectra
Abstract

We study the polarization properties of extragalactic sources at 95 and 150 GHz in the SPTpol 500 deg2 survey. We estimate the polarized power by stacking maps at known source positions, and correct for noise bias by subtracting the mean polarized power at random positions in the maps. We show that the method is unbiased using a set of simulated maps with similar noise properties to the real SPTpol maps. We find a flux-weighted mean-squared polarization fraction 〈 p 2〉 = [8.9 ± 1.1] × 10−4 at 95 GHz and [6.9 ± 1.1] × 10−4 at 150 GHz for the full sample. This is consistent with the values obtained for a subsample of active galactic nuclei. For dusty sources, we find 95 per cent upper limits of 〈 p 2〉95 < 16.9 × 10−3 and 〈 p 2〉150 < 2.6 × 10−3. We find no evidence that the polarization fraction depends on the source flux or observing frequency. The 1σ upper limit on measured mean-squared polarization fraction at 150 GHz implies that extragalactic foregrounds will be subdominant to the CMB E and B mode polarization power spectra out to at least ℓ ≲ 5700 (ℓ ≲ 4700) and ℓ ≲ 5300 (ℓ ≲ 3600), respectively, at 95 (150) GHz. [ABSTRACT FROM AUTHOR]

Published
2019
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5. Constraining radio mode feedback in galaxy clusters with the cluster radio AGNs properties to z ∼ 1

Author

Nikhel Gupta, Tesla E. Jeltema, X. Shao, C. Lidman, Santiago Avila, Vinu Vikram, Michael McDonald, E. Buckley-Geer, David J. Brooks, R. L. C. Ogando, Joseph J. Mohr, M. E. C. Swanson, D. L. Hollowood, V. Scarpine, Shantanu Desai, Maurilio Pannella, Peter Doel, S. Serrano, V. Strazzullo, I-Non Chiu, Matthias Klein, John P. Stott, Enrique Gaztanaga, Robert A. Gruendl, Michael Schubnell, Basilio X. Santiago, J. P. Dietrich, Juan Garcia-Bellido, E. Suchyta, Ramon Miquel, E. J. Sanchez, August E. Evrard, Marcos Lima, Rafe Schindler, J. Annis, Kyler Kuehn, Federico Bianchini, M. Costanzi, J. Gschwend, G. Gutierrez, Christian L. Reichardt, David J. James, A. Saro, Antonella Palmese, A. A. Plazas, L. N. da Costa, M. Smith, I. Sevilla-Noarbe, Daniel Gruen, M. A. G. Maia, S. Everett, F. Paz-Chinchón, J. de Vicente, Jennifer L. Marshall, Esra Bulbul, M. Carrasco Kind, Alfredo Zenteno, J. Carretero, Eli S. Rykoff, A. Carnero Rosell, K. Honscheid, Felipe Menanteau, Gupta, N., Pannella, M., Mohr, J. J., Klein, M., Rykoff, E. S., Annis, J., Avila, S., Bianchini, F., Brooks, D., Buckley-Geer, E., Bulbul, E., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Chiu, I., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Everett, S., Evrard, A. E., García-Bellido, J., Gaztanaga, E., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Lidman, C., Lima, M., Maia, M. A. G., Marshall, J. L., Mcdonald, M., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Reichardt, C. L., Sanchez, E., Santiago, B., Saro, A., Scarpine, V., Schindler, R., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Shao, X., Smith, M., Stott, J. P., Strazzullo, V., Suchyta, E., Swanson, M. E. C., Vikram, V., and Zenteno, A.

Subjects
submillimeter: galaxies, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Active galactic nucleus, Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, FOS: Physical sciences, galaxies [submillimeter], Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Luminosity, Intracluster medium, 0103 physical sciences, clusters: general [galaxies], 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Galaxy cluster, Luminosity function (astronomy), Physics, Astronomy and Astrophysics, luminosity function, mass function [galaxies], Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, galaxies: luminosity function, galaxies: clusters: general, mass function, Space and Planetary Science, cosmology: observations, Astrophysics of Galaxies (astro-ph.GA), active [galaxies], galaxies: luminosity function, mass function, High Energy Physics::Experiment, observation [cosmology], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We study the properties of the Sydney University Molonglo Sky Survey (SUMSS) 843~MHz radio AGN population in galaxy clusters from two large catalogs created using the Dark Energy Survey (DES): $\sim$11,800 optically selected RM-Y3 and $\sim$1,000 X-ray selected MARD-Y3 clusters. We show that cluster radio loud AGN are highly concentrated around cluster centers to $z\sim1$. We measure the halo occupation number for cluster radio AGN above a threshold luminosity, finding that the number of radio AGN per cluster increases with cluster halo mass as $N\propto M^{1.2\pm0.1}$ ($N\propto M^{0.68\pm0.34}$) for the RM-Y3 (MARD-Y3) sample. Together, these results indicate that radio mode feedback is favoured in more massive galaxy clusters. Using optical counterparts for these sources, we demonstrate weak redshift evolution in the host broad band colors and the radio luminosity at fixed host galaxy stellar mass. We use the redshift evolution in radio luminosity to break the degeneracy between density and luminosity evolution scenarios in the redshift trend of the radio AGN luminosity function (LF). The LF exhibits a redshift trend of the form $(1+z)^\gamma$ in density and luminosity, respectively, of $\gamma_{\rm D}=3.0\pm0.4$ and $\gamma_{\rm P}=0.21\pm0.15$ in the RM-Y3 sample, and $\gamma_{\rm D}=2.6\pm0.7$ and $\gamma_{\rm P}=0.31\pm0.15$ in MARD-Y3. We discuss the physical drivers of radio mode feedback in cluster AGN, and we use the cluster radio galaxy LF to estimate the average radio-mode feedback energy as a function of cluster mass and redshift and compare it to the core ($, Comment: 20 pages, 15 figures Replaced with published version

Published
2020

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