The Atacama Cosmology Telescope: Summary of DR4 and DR5 Data Products and Data Access

Mallaby-Kay, Maya; Atkins, Zachary; Aiola, Simone; Amodeo, Stefania; Austermann, J. E.; Beall, James A.; Becker, Daniel; Bond, J. Richard; Calabrese, E.; Chesmore, Grace E.; Choi, Steve K.; Crowley, Kevin T.; Darwish, Omar; Denison, E. V.; Devlin, Mark J.; Duff, Shannon M.; Duivenvoorden, Adriaan J.; Dunkley, Jo; Ferraro, Simone; Fichman, Kyra; Gallardo, Patricio A.; Golec, Joseph E.; Guan, Yilun; Han, Dongwon; Hasselfield, Matthew; Hill, J. Colin; Hilton, G. C.; Hilton, Matt; Hložek, Renée; Hubmayr, Johannes; Huffenberger, K. M.; Hughes, John P.; Koopman, Brian J.; Louis, Thibaut; MacInnis, Amanda; Madhavacheril, Mathew S.; McMahon, Jeff; Moodley, Kavilan; Næss, Sigurd; Namikawa, Toshiya; Nati, F.; Newburgh, Laura; Nibarger, J. P.; Niemack, Michael D.; Page, Lyman A.; Salatino, Maria; Schaan, Emmanuel; Schillaci, A.; Sehgal, Neelima; Sherwin, Blake D.; Sifón, Cristobál; Simon, Sara M.; Staggs, Suzanne T.; Storer, Émilie; Ullom, Joel N.; Engelen, Alexander van; Lanen, Jeff Van; Vale, Leila R.; Wollack, Edward J.; Xu, Zhilei

doi:10.3847/1538-4365/abfcc4

Cited by 27 publications

(21 citation statements)

References 37 publications

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“…CMB-type experiments have already mapped the millimetre sky over thousands of square degrees with beamsizes of around 1 arcmin (e.g. Mallaby-Kay et al 2021;Sobrin et al 2022) and the entire sky with Planck's 5-arcmin beam. In a few year's time, the Prime-Cam instrument on CCAT-prime/FYST (CCAT-Prime Collaboration 2021) will carry out a survey of 20,000 deg 2 of sky from Chile, over several millimetre-to-submillimetre bands, with a beamsize of 15 arcsec at 350 µm.…”

Section: Discussionmentioning

confidence: 99%

Constraints on galaxy formation from the cosmic-infrared-background$\,-\,$optical-imaging cross-correlation using $\boldsymbol{Herschel}$ and UNIONS

Lim¹,

Hill²,

Scott³

et al. 2022

Preprint

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Using Herschel-SPIRE imaging and the Canada-France Imaging Survey (CFIS) Low Surface Brightness data products from the Ultraviolet Near-Infrared Optical Northern Survey (UNIONS), we present a cross-correlation between the cosmic infrared background and cosmic optical background fluctuations. With a combined sky area of 91 deg 2 and a minimum resolved scale of 18 arcsec, the cross-spectrum is measured for two cases: all galaxies are kept in the images; or all individually-detected galaxies are masked to produce 'background' maps. We report the detection of the crosscorrelation signal at 22 σ ( 18 σ for the background map). The part of the optical brightness variations that are correlated with the submm emission translates to an rms brightness of 32.5 mag arcsec −2 in the r band, a level normally unreachable for individual sources. A critical issue is determining what fraction of the cross-power spectrum might be caused by emission from Galactic cirrus. For one of the fields, the Galactic contamination is approximately a factor of 10 higher than the extragalactic signal, with the contamination being estimated using a linear regression from several external survey maps; however, for the other fields, the contamination is typically around 20 per cent. An additional discriminant is that the cross-power spectrum is of the approximate form P (k) ∝ 1/k, much shallower than that of Galactic cirrus. We interpret the results in a halo-model framework, which shows good agreement with independent measurements for the scalings of star-formation rates in galaxies. The approach presented in this study holds great promise for future surveys such as FYST/CCAT-prime combined with Euclid or the Vera Rubin Observatory (LSST), which will enable a detailed exploration of the evolution of star formation in galaxies.

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Section: Discussionmentioning

confidence: 99%

Constraints on galaxy formation from the cosmic-infrared-background$\,-\,$optical-imaging cross-correlation using $\boldsymbol{Herschel}$ and UNIONS

Lim¹,

Hill²,

Scott³

et al. 2022

Preprint

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“…For instance, analysis with SPT-3G data would be interesting to test whether these results are 'ground-based experiment (in)dependent', or whether they could come from fluctuation in a given patch of the sky. In addition to this, the ACT collaboration already has data beyond DR4 (i.e., DR5 [59] which includes data acquired in 2017-18) which may also shed light on the DR4 preference for EDE cosmologies.…”

Section: Final Thoughtsmentioning

confidence: 99%

Dark Energy at early times and ACT: a larger Hubble constant without late-time priors

Poulin,

Smith,

Bartlett

2021

Preprint

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Recent observations using the Atacama Cosmology Telescope (ACT) have provided ground-based cosmic microwave background (CMB) maps with higher angular resolution than the Planck satellite. These have the potential to put interesting constraints on models resolving the 'Hubble tension'. In this paper we fit two models of Early Dark Energy (EDE) (an increase in the expansion rate around matter/radiation equality) to the combination of ACT data with large-scale measurements of the CMB either from the WMAP or the Planck satellite (including lensing), along with measurements of the baryon acoustic oscillations and uncalibrated supernovae luminosity distance. We study a phenomenological axion-like potential ('axEDE') and a scalar field experiencing a first-order phasetransition ('NEDE'). We find that for both models the 'Planck-free' analysis yields non-zero EDE at 2σ and an increased value for H0 ∼ 70 − 74 km/s/Mpc, compatible with local measurements, without the inclusion of any prior on H0. On the other hand, the inclusion of Planck data restricts the EDE contribution to an upper-limit only at 95% C.L. For axEDE, the combination of Planck and ACT leads to constraints 30% weaker than with Planck alone, and there is no residual Hubble tension. On the other hand, NEDE is more strongly constrained in a Planck+ACT analysis, and the Hubble tension remains at ∼ 3σ, illustrating the ability for CMB data to distinguish between different EDE models. We further explore the apparent inconsistency between the Planck and ACT data and find that it comes (mostly) from a slight tension between the temperature power spectrum at multipoles around ∼ 1000 and ∼ 1500. Finally, through a mock analysis of ACT data, we demonstrate that the preference for EDE is not driven by a lack of information at high-when removing Planck data, and that a ΛCDM fit to the fiducial EDE cosmology results in a significant bias on {H0, ω cdm }. More accurate measurements of the TT CMB power spectra above ∼ 2500 and EE between ∼ 300 − 500 will play a crucial role in differentiating between EDE models.

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“…crowave Background Data Analysis 31 (LAMBDA) and at the National Energy Research Scientific Computing Center (NERSC). Details of all these data products are given in Mallaby-Kay et al (2021).…”

Section: Leakage Correctionmentioning

confidence: 99%

“…Each year of data is referred to as a season (S13-S16) and was analyzed separately. The DR4 data products and some of their analyses are presented in Choi et al (2020), Aiola et al (2020), Darwish et al (2020), Han et al (2021), Madhavacheril et al (2020), Namikawa et al (2020), andMallaby-Kay et al (2021).…”

Section: Introductionmentioning

confidence: 99%

The Atacama Cosmology Telescope: measurement and analysis of 1D beams for DR4

Lungu

Storer

Hasselfield

et al. 2022

J. Cosmol. Astropart. Phys.

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We describe the measurement and treatment of the telescope beams for the Atacama Cosmology Telescope's fourth data release, DR4. Observations of Uranus are used to measure the central portion (<12') of the beams to roughly -40 dB of the peak. Such planet maps in intensity are used to construct azimuthally averaged beam profiles, which are fit with a physically motivated model before being transformed into Fourier space. We investigate and quantify a number of percent-level corrections to the beams, all of which are important for precision cosmology. Uranus maps in polarization are used to measure the temperature-to-polarization leakage in the main part of the beams, which is ≲ 1% (2.5%) at 150 GHz (98 GHz). The beams also have polarized sidelobes, which are measured with observations of Saturn and deprojected from the ACT time-ordered data. Notable changes relative to past ACT beam analyses include an improved subtraction of the atmospheric effects from Uranus calibration maps, incorporation of a scattering term in the beam profile model, and refinements to the beam model uncertainties and the main temperature-to-polarization leakage terms in the ACT power spectrum analysis.

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The Atacama Cosmology Telescope: Summary of DR4 and DR5 Data Products and Data Access

Cited by 27 publications

References 37 publications

Constraints on galaxy formation from the cosmic-infrared-background$\,-\,$optical-imaging cross-correlation using $\boldsymbol{Herschel}$ and UNIONS

Constraints on galaxy formation from the cosmic-infrared-background$\,-\,$optical-imaging cross-correlation using $\boldsymbol{Herschel}$ and UNIONS

Dark Energy at early times and ACT: a larger Hubble constant without late-time priors

The Atacama Cosmology Telescope: measurement and analysis of 1D beams for DR4

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