THE ATACAMA COSMOLOGY TELESCOPE: THE POLARIZATION-SENSITIVE ACTPol INSTRUMENT

Thornton, Robert J.; Ade, Peter A. R.; Aiola, Simone; Angilè, Francesco E.; Amiri, M.; Beall, James A.; Becker, D.; Cho, H-M.; Choi, Steve K.; Corlies, P.; Coughlin, Kevin; Datta, Rahul; Devlin, Mark J.; Dicker, Simon; Dünner, Rolando; Fowler, Joseph W.; Fox, Anna E.; Gallardo, Patricio A.; Gao, Jiansong; Grace, E.; Halpern, M.; Hasselfield, Matthew; Henderson, S.; Hilton, G. C.; Hincks, Adam D.; Ho, Shuay Pwu Patty; Hubmayr, Johannes; Irwin, K. D.; Klein, Jeff; Koopman, Brian J.; Li, Dale; Louis, Thibaut; Lungu, Marius; Maurin, Loïc; McMahon, Jeff; Munson, Charles; Næss, Sigurd; Nati, F.; Newburgh, Laura; Nibarger, J. P.; Niemack, Michael D.; Niraula, P.; Nolta, Michael R.; Page, Lyman A.; Pappas, Christine G.; Schillaci, A.; Schmitt, Benjamin L.; Sehgal, Neelima; Sievers, Jonathan; Simon, Sara M.; Staggs, Suzanne T.; Tucker, C.; Uehara, Masao; Lanen, Jeff Van; Ward, Jennifer E.; Wollack, Edward J.

doi:10.3847/1538-4365/227/2/21

Cited by 231 publications

(201 citation statements)

References 34 publications

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“…The second-generation ACT survey was conducted with the polarization-sensitive ACTPol receiver. The ACTPol survey took place from 2013-2015 in frequency bands 95 GHz and 148 GHz (Niemack et al 2010;Thornton et al 2016). Louis et al (2017) give a description of the ACTPol data reduction, calibration, and beams.…”

Section: Atacama Cosmology Telescope (Act)mentioning

confidence: 99%

“…The ACTPol calibrations have not yet been finalized and may change at the ∼1 per cent level, but our results in this paper are robust against these changes. More details of the ACTPol data and instrument can be found in Thornton et al (2016) and Louis et al (2017).…”

Section: Atacama Cosmology Telescope (Act)mentioning

confidence: 99%

“…This line enters the 95 GHz band between approximately z = 1 and z = 2. The 148 GHz ACTPol detectors have a bandwidths that are 51 GHz (first two detectors) and 41 GHz (third detector), while the ACT equatorial 148 GHz MBAC has a bandwidth of ∼18 GHz (Swetz et al 2011;Thornton et al 2016). In the lowest redshift bin, this makes the ACTPol 148 GHz data sensitive to the CO J (2-1) line emission between z = 0.35 − 0.87, and the ACT equatorial 148 GHz data are sensitive to it between z = 0.45−0.65.…”

Section: Modelling the Stacked Sedsmentioning

confidence: 99%

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Quantifying the thermal Sunyaev–Zel’dovich effect and excess millimetre emission in quasar environments

Hall

Zakamska

Addison

et al. 2019

Monthly Notices of the Royal Astronomical Society

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In this paper we probe the hot, post-shock gas component of quasar-driven winds through the thermal Sunyaev-Zel'dovich (tSZ) effect. Combining datasets from the Atacama Cosmology Telescope, the Herschel Space Observatory, and the Very Large Array, we measure average spectral energy distributions (SEDs) of 109,829 opticallyselected, radio quiet quasars from 1.4 GHz to 3000 GHz in six redshift bins between 0.3 < z < 3.5. We model the emission components in the radio and far-infrared, plus a spectral distortion from the tSZ effect. At z > 1.91, we measure the tSZ effect at 3.8σ significance with an amplitude corresponding to a total thermal energy of 3.1 × 10 60 ergs. If this energy is due to virialized gas, then our measurement implies quasar host halo masses are ∼ 6 × 10 12 h −1 M . Alternatively, if the host dark matter halo masses are ∼ 2 × 10 12 h −1 M as some measurements suggest, then we measure a >90 per cent excess in the thermal energy over that expected due to virialization. If the measured SZ effect is primarily due to hot bubbles from quasar-driven winds, we find that (5 +1.2 −1.3 ) per cent of the quasar bolometric luminosity couples to the intergalactic medium over a fiducial quasar lifetime of 100 Myr. An additional source of tSZ may be correlated structure, and further work is required to separate the contributions. At z ≤ 1.91, we detect emission at 95 and 148 GHz that is in excess of thermal dust and optically thin synchrotron emission. We investigate potential sources of this excess emission, finding that CO line emission and an additional optically thick synchrotron component are the most viable candidates.

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Section: Atacama Cosmology Telescope (Act)mentioning

confidence: 99%

Section: Atacama Cosmology Telescope (Act)mentioning

confidence: 99%

Section: Modelling the Stacked Sedsmentioning

confidence: 99%

See 1 more Smart Citation

Quantifying the thermal Sunyaev–Zel’dovich effect and excess millimetre emission in quasar environments

Hall

Zakamska

Addison

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…Given the moderate internal Planck tension in these parameters, it is informative to consider other CMB measurements to help understand the extent to which conclusions are driven by Planck data, or are independent of Planck. In this work we therefore also include results from the final WMAP 9-year analysis (Bennett et al 2013;Hinshaw et al 2013), the Atacama Cosmology Telescope polarization-sensitive receiver (ACTPol; Thornton et al 2016;Louis et al 2017;Sherwin et al 2016) two-season survey, covering 548 deg 2 , and the 2500 deg 2 South Pole Telescope Sunyaev-Zel'dovich survey (SPT-SZ; Carlstrom et al 2011;Story et al 2013;van Engelen et al 2012). …”

Section: Choice Of Cmb Data For Joint Fitsmentioning

confidence: 99%

Elucidating ΛCDM: Impact of Baryon Acoustic Oscillation Measurements on the Hubble Constant Discrepancy

Addison¹,

Watts²,

Bennett³

et al. 2018

ApJ

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253

209

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We examine the impact of baryon acoustic oscillation (BAO) scale measurements on the discrepancy between the value of the Hubble constant (H 0 ) inferred from the local distance ladder and from Planck cosmic microwave background (CMB) data. While the BAO data alone cannot constrain H 0 , we show that combining the latest BAO results with WMAP, Atacama Cosmology Telescope (ACT), or South Pole Telescope (SPT) CMB data produces values of H 0 that are 2.4 − 3.1σ lower than the distance ladder, independent of Planck, and that this downward pull was less apparent in some earlier analyses that used only angle-averaged BAO scale constraints rather than full anisotropic information. At the same time, the combination of BAO and CMB data also disfavors the lower values of H 0 preferred by the Planck high-multipole temperature power spectrum. Combining galaxy and Lyman-α forest (Lyα) BAO with a precise estimate of the primordial deuterium abundance produces H 0 = 66.98 ± 1.18 km s −1 Mpc −1 for the flat ΛCDM model. This value is completely independent of CMB anisotropy constraints and is 3.0σ lower than the latest distance ladder constraint, although 2.4σ tension also exists between the galaxy BAO and Lyα BAO. These results show that it is not possible to explain the H 0 disagreement solely with a systematic error specific to the Planck data. The fact that tensions remain even after the removal of any single data set makes this intriguing puzzle all the more challenging to resolve.

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“…The fields should overlap other multi-wavelength datasets to maximize scientific outputs when combined with the HSC data. The major datasets that offer unique synergy with HSC data are the arc-minute-resolution, high-sensitivity CMB survey by the Atacama Cosmology Telescope (ACT; Swetz et al 2011) in Chile, and its polarization extension ACTPol (Thornton et al 2016); X-ray data from XMM-XXL (Pierre et al 2016) and eROSITA 8 ; near-/mid-infrared imaging surveys (e.g., VIKING/VIDEO 9 and UKIDSS 10 ); and deep spectroscopic surveys such as VVDS (Le Fèvre et al 2013), DEEP2 11 , zCOSMOS 12 , VIPERS 13 , GAMA 14 , HectoMap (Hwang et al 2016), and AEGIS (Davis et al 2007). Finally, the fields should be low in Galactic dust extinction and as spatially continuous as possible, to enable cosmological analysis on large scales.…”

Section: First Year Datasetmentioning

confidence: 99%

The first-year shear catalog of the Subaru Hyper Suprime-Cam Subaru Strategic Program Survey

Mandelbaum

Miyatake

Hamana

et al. 2017

Publications of the Astronomical Society of Japan

224

195

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We present and characterize the catalog of galaxy shape measurements that will be used for cosmological weak lensing measurements in the Wide layer of the first year of the Hyper Suprime-Cam (HSC) survey. The catalog covers an area of 136.9 deg 2 split into six fields, with a mean i-band seeing of 0.58 ′′ and 5σ point-source depth of i ∼ 26. Given conservative galaxy selection criteria for first year science, the depth and excellent image quality results in unweighted and weighted source number densities of 24.6 and 21.8 arcmin −2 , respectively. We define the requirements for cosmological weak lensing science with this catalog, then focus on characterizing potential systematics in the catalog using a series of internal null tests for problems with point-spread function (PSF) modeling, shear estimation, and other aspects of the image processing. We find that the PSF models narrowly meet requirements for weak lensing science with this catalog, with fractional PSF model size residuals of approximately 0.003 (requirement: 0.004) and the PSF model shape correlation function ρ 1 < 3 × 10 −7 (requirement:A variety of galaxy shape-related null tests are statistically consistent with zero, but star-galaxy shape correlations reveal additive systematics on on > 1• scales that are sufficiently large as to require mitigation in cosmic shear measurements. Finally, we discuss the dominant systematics and the planned algorithmic changes to reduce them in future data reductions.

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THE ATACAMA COSMOLOGY TELESCOPE: THE POLARIZATION-SENSITIVE ACTPol INSTRUMENT

Cited by 231 publications

References 34 publications

Quantifying the thermal Sunyaev–Zel’dovich effect and excess millimetre emission in quasar environments

Quantifying the thermal Sunyaev–Zel’dovich effect and excess millimetre emission in quasar environments

Elucidating ΛCDM: Impact of Baryon Acoustic Oscillation Measurements on the Hubble Constant Discrepancy

The first-year shear catalog of the Subaru Hyper Suprime-Cam Subaru Strategic Program Survey

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