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1. Fabrication and characterization of optical filters from polymeric aerogels loaded with diamond scattering particles

Author: Barlis, Alyssa, Guo, Haiquan, Helson, Kyle, Bennett, Charles, Chan, Yan Yan, Marriage, Tobias, Quijada, Manuel, Tokarz, Ariel, Vivod, Stephanie, Wollack, Edward, Essinger-Hileman, Thomas, Barlis, Alyssa, Guo, Haiquan, Helson, Kyle, Bennett, Charles, Chan, Yan Yan, Marriage, Tobias, Quijada, Manuel, Tokarz, Ariel, Vivod, Stephanie, Wollack, Edward, and Essinger-Hileman, Thomas
Abstract: We have developed a suite of infrared-blocking filters made by embedding diamond scattering particles in a polyimide aerogel substrate. We demonstrate the ability to tune the spectral performance of the filters based on both the composition of the base aerogel material and the properties of the scattering particles. We summarize the fabrication, optical modeling, and characterization of these filters. We investigate two polyimide base aerogel formulations and the effects of loading them with diamond scattering particles of varying sizes and relative densities. We describe a model for the filters' behavior using a combination of Maxwell Garnett and Mie Scattering techniques. We present optical characterization results for diamond-loaded aerogel filters with cutoff frequencies (50% transmittance) ranging between 2.5 and 15 THz, and confirm that the measured spectral performance is in agreement with our optical models. We also measure the filters' refractive index in the microwave and report findings in agreement with Maxwell Garnett model predictions (typically n < 1.08)., Comment: 18 pages, 11 figures, 3 tables. Submitted to Applied Optics
Published: 2024

2. Revisiting the $A_L$ Lensing Anomaly in Planck 2018 Temperature Data

Author: Addison, Graeme E., Bennett, Charles L., Halpern, Mark, Hinshaw, Gary, Weiland, Janet L., Addison, Graeme E., Bennett, Charles L., Halpern, Mark, Hinshaw, Gary, and Weiland, Janet L.
Abstract: We revisit the lensing anomaly in the Planck 2018 temperature (TT) data and examine its robustness to frequency selection and additional sky masking. Our main findings are: (1) The phenomenological lensing amplitude parameter, $A_L$, varies with ecliptic latitude, with a $2.9\sigma$ preference for $A_L>1$ near the ecliptic, and $1.0\sigma$ preference near the ecliptic poles, compared to $2.5\sigma$ on the original masks. This behavior is largely or solely from 217 GHz and suggestive of some non-random effect given the Planck scan strategy. (2) The 217 GHz TT data also show a stronger preference for $A_L>1$ than the lower frequencies. The shifts in $A_L$ from 217 GHz with additional Galactic dust masking are too large to be explained solely by statistical fluctuations, indicating some connection with the foreground treatment. Overall, the Planck $A_L$ anomaly does not have a single simple cause. Removing the 217 GHz TT data leaves a $1.8\sigma$ preference for $A_L>1$. The low-multipole ($\ell<30$) TT data contribute to the preference for $A_L>1$ through correlations with $\Lambda$CDM parameters. The 100 and 143 GHz data at $\ell\geq30$ prefer $A_L>1$ at $1.3\sigma$, and this appears robust to the masking tests we performed. The lensing anomaly may impact fits to alternative cosmological models. Marginalizing over $A_L$, optionally applied only to Planck TT spectra, can check this. Models proposed to address cosmological tensions should be robust to removal of the Planck 217 GHz TT data., Comment: 27 pages, 10 figures, submitted to ApJ
Published: 2023

3. CLASS Observations of Atmospheric Cloud Polarization at Millimeter Wavelengths

Author: Li, Yunyang, Appel, John W., Bennett, Charles L., Bustos, Ricardo, Chuss, David T., Cleary, Joseph, Couto, Jullianna Denes, Dahal, Sumit, Datta, Rahul, Dünner, Rolando, Eimer, Joseph R., Essinger-Hileman, Thomas, Harrington, Kathleen, Iuliano, Jeffrey, Marriage, Tobias A., Petroff, Matthew A., Reeves, Rodrigo A., Rostem, Karwan, Shi, Rui, Valle, Deniz A. N., Watts, Duncan J., Wolff, Oliver F., Wollack, Edward J., Xu, Zhilei, Li, Yunyang, Appel, John W., Bennett, Charles L., Bustos, Ricardo, Chuss, David T., Cleary, Joseph, Couto, Jullianna Denes, Dahal, Sumit, Datta, Rahul, Dünner, Rolando, Eimer, Joseph R., Essinger-Hileman, Thomas, Harrington, Kathleen, Iuliano, Jeffrey, Marriage, Tobias A., Petroff, Matthew A., Reeves, Rodrigo A., Rostem, Karwan, Shi, Rui, Valle, Deniz A. N., Watts, Duncan J., Wolff, Oliver F., Wollack, Edward J., and Xu, Zhilei
Abstract: The dynamic atmosphere imposes challenges to ground-based cosmic microwave background observation, especially for measurements on large angular scales. The hydrometeors in the atmosphere, mostly in the form of clouds, scatter the ambient thermal radiation and are known to be the main linearly polarized source in the atmosphere. This scattering-induced polarization is significantly enhanced for ice clouds due to the alignment of ice crystals under gravity, which are also the most common clouds seen at the millimeter-astronomy sites at high altitudes. This work presents a multifrequency study of cloud polarization observed by the Cosmology Large Angular Scale Surveyor (CLASS) experiment on Cerro Toco in the Atacama Desert of northern Chile, from 2016 to 2022, at the frequency bands centered around 40, 90, 150, and 220 GHz. Using a machine-learning-assisted cloud classifier, we made connections between the transient polarized emission found in all four frequencies with the clouds imaged by monitoring cameras at the observing site. The polarization angles of the cloud events are found to be mostly $90^\circ$ from the local meridian, which is consistent with the presence of horizontally aligned ice crystals. The 90 and 150 GHz polarization data are consistent with a power law with a spectral index of $3.90\pm0.06$, while an excess/deficit of polarization amplitude is found at 40/220 GHz compared with a Rayleigh scattering spectrum. These results are consistent with Rayleigh-scattering-dominated cloud polarization, with possible effects from supercooled water absorption and/or Mie scattering from a population of large cloud particles that contribute to the 220 GHz polarization., Comment: 16 pages, 14 figures, submitted to ApJ
Published: 2023

4. CLASS Angular Power Spectra and Map-Component Analysis for 40 GHz Observations through 2022

Author: Eimer, Joseph R., Li, Yunyang, Brewer, Michael K., Shi, Rui, Ali, Aamir, Appel, John W., Bennett, Charles L., Bruno, Sarah Marie, Bustos, Ricardo, Chuss, David T., Cleary, Joseph, Dahal, Sumit, Datta, Rahul, Couto, Jullianna Denes, Denis, Kevin L., Dünner, Rolando, Essinger-Hileman, Thomas, Fluxá, Pedro, Hubmayer, Johannes, Harrington, Kathleen, Iuliano, Jeffrey, Karakla, John, Marriage, Tobias A., Núñez, Carolina, Parker, Lucas, Petroff, Matthew A., Reeves, Rodrigo A., Rostem, Karwan, Valle, Deniz A. N., Watts, Duncan J., Weiland, Janet L., Wollack, Edward J., Xu, Zhilei, Zeng, Lingzhen, Eimer, Joseph R., Li, Yunyang, Brewer, Michael K., Shi, Rui, Ali, Aamir, Appel, John W., Bennett, Charles L., Bruno, Sarah Marie, Bustos, Ricardo, Chuss, David T., Cleary, Joseph, Dahal, Sumit, Datta, Rahul, Couto, Jullianna Denes, Denis, Kevin L., Dünner, Rolando, Essinger-Hileman, Thomas, Fluxá, Pedro, Hubmayer, Johannes, Harrington, Kathleen, Iuliano, Jeffrey, Karakla, John, Marriage, Tobias A., Núñez, Carolina, Parker, Lucas, Petroff, Matthew A., Reeves, Rodrigo A., Rostem, Karwan, Valle, Deniz A. N., Watts, Duncan J., Weiland, Janet L., Wollack, Edward J., Xu, Zhilei, and Zeng, Lingzhen
Abstract: Measurement of the largest angular scale ($\ell < 30$) features of the cosmic microwave background (CMB) polarization is a powerful way to constrain the optical depth to reionization and search for the signature of inflation through the detection of primordial $B$-modes. We present an analysis of maps covering 73.6\% of the sky made from the $40\,\mathrm{GHz}$ channel of the Cosmology Large Angular Scale Surveyor (CLASS) from 2016 August to 2022 May. Taking advantage of the measurement stability enabled by front-end polarization modulation and excellent conditions from the Atacama Desert, we show this channel achieves higher sensitivity than the analogous frequencies from satellite measurements in the range $10 < \ell < 100$. Simulations show the CLASS linear (circular) polarization maps have a white noise level of $125 \,(130)\,\mathrm{\mu K\, arcmin}$. We measure the Galaxy-masked $EE$ and $BB$ spectra of diffuse synchrotron radiation and compare to space-based measurements at similar frequencies. In combination with external data, we expand measurements of the spatial variations of the synchrotron spectral energy density (SED) to include new sky regions and measure the diffuse SED in the harmonic domain. We place a new upper limit on a background of circular polarization in the range $5 < \ell < 125$ with the first bin showing $D_\ell < 0.023$ $\mathrm{\mu K^2_{CMB}}$ at 95\% confidence. These results establish a new standard for recovery of the largest-scale CMB polarization from the ground and signal exciting possibilities when the higher sensitivity and higher-frequency CLASS channels are included in the analysis., Comment: 38 pages, 25 figures, 6 tables. Accepted to The Astrophysical Journal
Published: 2023

5. Cosmology Large Angular Scale Surveyor (CLASS): 90 GHz Telescope Pointing, Beam Profile, Window Function, and Polarization Performance

Author: Datta, Rahul, Brewer, Michael K., Couto, Jullianna Denes, Eimer, Joseph, Li, Yunyang, Xu, Zhilei, Ali, Aamir, Appel, John W., Bennett, Charles L., Bustos, Ricardo, Chuss, David T., Cleary, Joseph, Dahal, Sumit, Espinoza, Francisco, Essinger-Hileman, Thomas, Fluxá, Pedro, Harrington, Kathleen, Helson, Kyle, Iuliano, Jeffrey, Karakla, John, Marriage, Tobias A., Novack, Sasha, Núñez, Carolina, Padilla, Ivan L., Parker, Lucas, Petroff, Matthew A., Reeves, Rodrigo, Rostem, Karwan, Shi, Rui, Valle, Deniz A. N., Watts, Duncan J., Weiland, Janet L., Wollack, Edward J., Zeng, Lingzhen, Datta, Rahul, Brewer, Michael K., Couto, Jullianna Denes, Eimer, Joseph, Li, Yunyang, Xu, Zhilei, Ali, Aamir, Appel, John W., Bennett, Charles L., Bustos, Ricardo, Chuss, David T., Cleary, Joseph, Dahal, Sumit, Espinoza, Francisco, Essinger-Hileman, Thomas, Fluxá, Pedro, Harrington, Kathleen, Helson, Kyle, Iuliano, Jeffrey, Karakla, John, Marriage, Tobias A., Novack, Sasha, Núñez, Carolina, Padilla, Ivan L., Parker, Lucas, Petroff, Matthew A., Reeves, Rodrigo, Rostem, Karwan, Shi, Rui, Valle, Deniz A. N., Watts, Duncan J., Weiland, Janet L., Wollack, Edward J., and Zeng, Lingzhen
Abstract: The Cosmology Large Angular Scale Surveyor (CLASS) is a telescope array that observes the cosmic microwave background (CMB) over ~75% of the sky from the Atacama Desert, Chile, at frequency bands centered near 40, 90, 150, and 220 GHz. CLASS measures the large angular scale CMB polarization to constrain the tensor-to-scalar ratio and the optical depth to last scattering. This paper presents the optical characterization of the 90GHz telescope, which has been observing since July 2018. Observations of the Moon establish the pointing while dedicated observations of Jupiter are used for beam calibration. The standard deviations of the pointing error in azimuth, elevation, and boresight angle are 1.3, 2.1, and 2.0 arcminutes, respectively, over the first 3 years of observations. This corresponds to a pointing uncertainty ~7% of the beam's full width at half maximum (FWHM). The effective azimuthally-symmetrized 1D beam estimated at 90 GHz from per detector intensity beam maps has a FWHM of 0.614+/-0.003 deg and a solid angle of 136.3+/-0.6(stats.)+/-1.1(sys.) usr integrated to a radius of 4 deg. The corresponding beam window function drops to b_ell^2 = 0.92, 0.70, 0.14 at ell = 30, 100, 300, respectively, with relative uncertainties < 2% for ell < 200. Far-sidelobes are studied using detector-centered intensity maps of the Moon and measured to be at a level of 10^-3 or below relative to the peak. The polarization angle of Tau A estimated from preliminary survey maps is 149.6+/-0.2(stats.) deg in equatorial coordinates consistent with prior measurements. Instrumental temperature-to-polarization (T-to-P) leakage is measured at a 95% confidence upper limit of (1.7+/-0.1) x 10^-3 in single detector demodulated data using observations of Jupiter and the Moon. Using pair-differenced demodulated data, a 95% confidence upper limit of 3.6 x 10^-4 is obtained on the T-to-P leakage., Comment: 24 pages, 18 figures, submitted to ApJS
Published: 2023

6. Cosmological Tensions and the Transitional Planck Mass Model

Author: Kable, Joshua A, Benevento, Giampaolo, Addison, Graeme E, Bennett, Charles L, Kable, Joshua A, Benevento, Giampaolo, Addison, Graeme E, and Bennett, Charles L
Abstract: In this followup analysis, we update previous constraints on the Transitional Planck Mass (TPM) modified gravity model using the latest version of EFTCAMB and provide new constraints using SPT and Planck anisotropy data along with Planck CMB lensing, BAO, SNe Ia, and an $H_0$ prior from local measurements. We find that large shifts in the Planck mass lead to large suppression of power on small scales that is disfavored by both SPT and Planck. Using only SPT TE-EE data, this suppression of power can be compensated for by an upward shift of the scalar index to $n_s = 1.003 \pm 0.016$ resulting in $H_0 = 71.94^{+0.86}_{-0.85}$ kms$^{-1}$Mpc$^{-1}$ and a $\sim7\%$ shift in the Planck mass. Including Planck TT $\ell \leq 650$ and Planck TE-EE data restricts the shift to be $<5\%$ at $2\sigma$ with $H_0 = 70.65 \pm 0.66$ kms$^{-1}$Mpc$^{-1}$. Excluding the $H_0$ prior, SPT and Planck data constrain the shift in the Planck mass to be $<3\%$ at $2\sigma$ with a best-fit value of $0.04\%$, consistent with the $\Lambda$CDM limit. In this case $H_0 = 69.09^{+0.69}_{-0.68}$ kms$^{-1}$Mpc$^{-1}$, which is partially elevated by the dynamics of the scalar-field in the late universe. This differs from EDE models that prefer higher values of $H_0$ when high $\ell$ Planck TT data are excluded. We additionally constrain TPM using RSD data from BOSS DR 12 and cosmic shear, galaxy-galaxy lensing, and galaxy clustering data from DES Y1 finding both disfavor transitions close to recombination, but earlier Planck mass transitions are allowed., Comment: 25 pages, 8 figures, 8 tables
Published: 2023

7. CLASS Data Pipeline and Maps for 40 GHz Observations through 2022

Author: Li, Yunyang, Eimer, Joseph, Osumi, Keisuke, Appel, John, Brewer, Michael, Ali, Aamir, Bennett, Charles, Bruno, Sarah Marie, Bustos, Ricardo, Chuss, David, Cleary, Joseph, Couto, Jullianna, Dahal, Sumit, Datta, Rahul, Denis, Kevin, Dunner, Rolando, Inostroza, Francisco Raul Espinoza, Essinger-Hileman, Thomas, Fluxa, Pedro, Harrington, Kathleen, Iuliano, Jeffrey, Karakla, John, Marriage, Tobias, Miller, Nathan, Novack, Sasha, Núñez, Carolina, Petroff, Matthew, Reeves, Rodrigo, Rostem, Karwan, Shi, Rui, Valle, Deniz, Watts, Duncan, Weiland, J., Wollack, Edward, Xu, Zhilei, Zeng, Lingzhen, Li, Yunyang, Eimer, Joseph, Osumi, Keisuke, Appel, John, Brewer, Michael, Ali, Aamir, Bennett, Charles, Bruno, Sarah Marie, Bustos, Ricardo, Chuss, David, Cleary, Joseph, Couto, Jullianna, Dahal, Sumit, Datta, Rahul, Denis, Kevin, Dunner, Rolando, Inostroza, Francisco Raul Espinoza, Essinger-Hileman, Thomas, Fluxa, Pedro, Harrington, Kathleen, Iuliano, Jeffrey, Karakla, John, Marriage, Tobias, Miller, Nathan, Novack, Sasha, Núñez, Carolina, Petroff, Matthew, Reeves, Rodrigo, Rostem, Karwan, Shi, Rui, Valle, Deniz, Watts, Duncan, Weiland, J., Wollack, Edward, Xu, Zhilei, and Zeng, Lingzhen
Abstract: The Cosmology Large Angular Scale Surveyor (CLASS) is a telescope array that observes the cosmic microwave background over 75\% of the sky from the Atacama Desert, Chile, at frequency bands centered near 40, 90, 150, and 220~GHz. This paper describes the CLASS data pipeline and maps for 40~GHz observations conducted from August 2016 to May 2022. We demonstrate how well the CLASS survey strategy, with rapid ($\sim10\,\mathrm{Hz}$) front-end modulation, recovers the large-scale Galactic polarization signal from the ground: the mapping transfer function recovers $\sim75$\% of $EE$, $BB$, and $VV$ power at $\ell=20$ and $\sim45$\% at $\ell=10$. We present linear and circular polarization maps over 75\% of the sky. Simulations based on the data imply the maps have a white noise level of $110\,\mathrm{\mu K\, arcmin}$ and correlated noise component rising at low-$\ell$ as $\ell^{-2.2}$. The transfer-function-corrected low-$\ell$ component is comparable to the white noise at the angular knee frequencies of $\ell\approx16$ (linear polarization) and $\ell\approx12$ (circular polarization). Finally, we present simulations of the level at which expected sources of systematic error bias the measurements, finding sub-percent bias for the $\Lambda\mathrm{CDM}$ $EE$ power spectra. Bias from $E$-to-$B$ leakage due to the data reduction pipeline and polarization angle uncertainty approaches the expected level for an $r=0.01$ $BB$ power spectrum. Improvements to the instrument calibration and the data pipeline will decrease this bias., Comment: 29 pages, 17 figures; submitted to ApJ
Published: 2023

8. Microwave Observations of Venus with CLASS

Author: Dahal, Sumit, Brewer, Michael K., Akins, Alex B., Appel, John W., Bennett, Charles L., Bustos, Ricardo, Cleary, Joseph, Couto, Jullianna D., Datta, Rahul, Eimer, Joseph, Essinger-Hileman, Thomas, Iuliano, Jeffrey, Li, Yunyang, Marriage, Tobias A., Núñez, Carolina, Petroff, Matthew A., Reeves, Rodrigo, Rostem, Karwan, Shi, Rui, Valle, Deniz A. N., Watts, Duncan J., Weiland, Janet L., Wollack, Edward J., Xu, Zhilei, Dahal, Sumit, Brewer, Michael K., Akins, Alex B., Appel, John W., Bennett, Charles L., Bustos, Ricardo, Cleary, Joseph, Couto, Jullianna D., Datta, Rahul, Eimer, Joseph, Essinger-Hileman, Thomas, Iuliano, Jeffrey, Li, Yunyang, Marriage, Tobias A., Núñez, Carolina, Petroff, Matthew A., Reeves, Rodrigo, Rostem, Karwan, Shi, Rui, Valle, Deniz A. N., Watts, Duncan J., Weiland, Janet L., Wollack, Edward J., and Xu, Zhilei
Abstract: We report on the disk-averaged absolute brightness temperatures of Venus measured at four microwave frequency bands with the Cosmology Large Angular Scale Surveyor (CLASS). We measure temperatures of 432.3 $\pm$ 2.8 K, 355.6 $\pm$ 1.3 K, 317.9 $\pm$ 1.7 K, and 294.7 $\pm$ 1.9 K for frequency bands centered at 38.8, 93.7, 147.9, and 217.5 GHz, respectively. We do not observe any dependence of the measured brightness temperatures on solar illumination for all four frequency bands. A joint analysis of our measurements with lower frequency Very Large Array (VLA) observations suggests relatively warmer ($\sim$ 7 K higher) mean atmospheric temperatures and lower abundances of microwave continuum absorbers than those inferred from prior radio occultation measurements., Comment: 10 pages, 3 figures, published in PSJ
Published: 2023
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9. Cellular Automata '86 Conference

Author: Bennett, Charles H., Toffoli, Tommaso, Wolfram, Stephen, Bennett, Charles H., Toffoli, Tommaso, and Wolfram, Stephen
Published: 2023

10. On-sky performance of new 90 GHz detectors for the Cosmology Large Angular Scale Surveyor (CLASS)

Author: Núñez, Carolina, Appel, John W., Brewer, Michael K., Bruno, Sarah Marie, Datta, Rahul, Bennett, Charles L., Bustos, Ricardo, Chuss, David T., Dahal, Sumit, Denis, Kevin L., Eimer, Joseph, Essinger-Hileman, Thomas, Helson, Kyle, Marriage, Tobias, Pérez, Carolina Morales, Padilla, Ivan L., Petroff, Matthew A., Rostem, Karwan, Watts, Duncan J., Wollack, Edward J., Xu, Zhilei, Núñez, Carolina, Appel, John W., Brewer, Michael K., Bruno, Sarah Marie, Datta, Rahul, Bennett, Charles L., Bustos, Ricardo, Chuss, David T., Dahal, Sumit, Denis, Kevin L., Eimer, Joseph, Essinger-Hileman, Thomas, Helson, Kyle, Marriage, Tobias, Pérez, Carolina Morales, Padilla, Ivan L., Petroff, Matthew A., Rostem, Karwan, Watts, Duncan J., Wollack, Edward J., and Xu, Zhilei
Abstract: The Cosmology Large Angular Scale Surveyor (CLASS) is a polarization-sensitive telescope array located at an altitude of 5,200 m in the Chilean Atacama Desert and designed to measure the polarized Cosmic Microwave Background (CMB) over large angular scales. The CLASS array is currently observing with three telescopes covering four frequency bands: one at 40 GHz (Q); one at 90 GHz (W1); and one dichroic system at 150/220 GHz (HF). During the austral winter of 2022, we upgraded the first 90 GHz telescope (W1) by replacing four of the seven focal plane modules. These new modules contain detector wafers with an updated design, aimed at improving the optical efficiency and detector stability. We present a description of the design changes and measurements of on-sky optical efficiencies derived from observations of Jupiter., Comment: 5 pages, 3 figures, to appear in the IEEE Transactions on Applied Superconductivity. arXiv admin note: text overlap with arXiv:2208.05006
Published: 2023
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11. Polarized Synchrotron Foreground Assessment for CMB Experiments

Author: Weiland, Janet L., Addison, Graeme E., Bennett, Charles L., Halpern, Mark, Hinshaw, Gary, Weiland, Janet L., Addison, Graeme E., Bennett, Charles L., Halpern, Mark, and Hinshaw, Gary
Abstract: Polarized Galactic synchrotron emission is an undesirable foreground for cosmic microwave background (CMB) experiments observing at frequencies $< 150$ GHz. We perform a combined analysis of observational data at 1.4, 2.3, 23, 30 and 33 GHz to quantify the spatial variation of the polarized synchrotron spectral index, $\beta^{pol}$, on $\sim3.5^\circ$ scales. We compare results from different data combinations to address limitations and inconsistencies present in these public data, and form a composite map of $\beta^{pol}$. Data quality masking leaves 44% sky coverage (75% for $|b|> 45^\circ$). Generally $-3.2 < \beta^{pol} \lesssim -3$ in the inner Galactic plane and spurs, but the Fan Region in the outer Galaxy has a flatter index. We find a clear spectral index steepening with increasing latitude south of the Galactic plane with $\Delta \beta^{pol}=0.4$, and a smaller steepening of $0.25$ in the north. Near the south Galactic pole the polarized synchrotron spectral index is $\beta^{pol} \approx -3.4$. Longitudinal spectral index variations of $\Delta \beta^{pol} \sim 0.1$ about the latitudinal mean are also detected. Within the BICEP2/Keck survey footprint, we find consistency with a constant value, $\beta^{pol} = -3.25 \pm 0.04$ (statistical) $\pm 0.02$ (systematic). We compute a map of the frequency at which synchrotron and thermal dust emission contribute equally to the total polarized foreground. The limitations and inconsistencies among datasets encountered in this work make clear the value of additional independent surveys at multiple frequencies, especially between $10-20$ GHz, provided these surveys have sufficient sensitivity and control of instrumental systematic errors., Comment: 19 pages, 18 figures, submitted to ApJ
Published: 2022

12. Snowmass2021 Cosmic Frontier: Cosmic Microwave Background Measurements White Paper

Author: Chang, Clarence L., Huffenberger, Kevin M., Benson, Bradford A., Bianchini, Federico, Chluba, Jens, Delabrouille, Jacques, Flauger, Raphael, Hanany, Shaul, Jones, William C., Kogut, Alan J., McMahon, Jeffrey J., Meyers, Joel, Sehgal, Neelima, Simon, Sara M., Umilta, Caterina, Abazajian, Kevork N., Ahmed, Zeeshan, Akrami, Yashar, Anderson, Adam J., Ansarinejad, Behzad, Austermann, Jason, Baccigalupi, Carlo, Barkats, Denis, Barron, Darcy, Barry, Peter S., Battaglia, Nicholas, Baxter, Eric, Beck, Dominic, Bender, Amy N., Bennett, Charles, Beringue, Benjamin, Bischoff, Colin, Bleem, Lindsey, Bock, James, Bolliet, Boris, Bond, J Richard, Borrill, Julian, Brinckmann, Thejs, Brown, Michael L., Calabrese, Erminia, Carlstrom, John, Challinor, Anthony, Chang, Chihway, Chinone, Yuji, Clark, Susan E., Coulton, William, Cukierman, Ari, Cyr-Racine, Francis-Yan, Duff, Shannon M., Dvorkin, Cora, van Engelen, Alexander, Errard, Josquin, Eskilt, Johannes R., Essinger-Hileman, Thomas, Fabbian, Giulio, Feng, Chang, Ferraro, Simone, Filippini, Jeffrey, Freese, Katherine, Galitzki, Nicholas, Gawiser, Eric, Grin, Daniel, Grohs, Evan, Gruppuso, Alessandro, Gudmundsson, Jon E., Halverson, Nils W., Hamilton, Jean-Christophe, Harrington, Kathleen, Henrot-Versillé, Sophie, Hensley, Brandon, Hill, J. Colin, Hincks, Adam D., Hlozek, Renee, Holzapfel, William, Hotinli, Selim C., Hui, Howard, Ibitoye, Ayodeji, Johnson, Matthew, Johnson, Bradley R., Kang, Jae Hwan, Karkare, Kirit S., Knox, Lloyd, Kovac, John, Lau, Kenny, Legrand, Louis, Loverde, Marilena, Lubin, Philip, Ma, Yin-Zhe, Mroczkowski, Tony, Mukherjee, Suvodip, Münchmeyer, Moritz, Nagai, Daisuke, Nagy, Johanna, Niemack, Michael, Novosad, Valentine, Omori, Yuuki, Orlando, Giorgio, Pan, Zhaodi, Perotto, Laurence, Petroff, Matthew A., Pogosian, Levon, Pryke, Clem, Rahlin, Alexandra, Raveri, Marco, Reichardt, Christian L., Remazeilles, Mathieu, Rephaeli, Yoel, Ruhl, John, Schaan, Emmanuel, Shandera, Sarah, Shimon, Meir, Soliman, Ahmed, Stark, Antony A., Starkman, Glenn D., Stompor, Radek, Thakur, Ritoban Basu, Trendafilova, Cynthia, Tristram, Matthieu, Trivedi, Pranjal, Tucker, Gregory, Di Valentino, Eleonora, Vieira, Joaquin, Vieregg, Abigail, Wang, Gensheng, Watson, Scott, Wenzl, Lukas, Wollack, Edward J., Wu, W. L. Kimmy, Xu, Zhilei, Zegeye, David, Zhang, Cheng, Chang, Clarence L., Huffenberger, Kevin M., Benson, Bradford A., Bianchini, Federico, Chluba, Jens, Delabrouille, Jacques, Flauger, Raphael, Hanany, Shaul, Jones, William C., Kogut, Alan J., McMahon, Jeffrey J., Meyers, Joel, Sehgal, Neelima, Simon, Sara M., Umilta, Caterina, Abazajian, Kevork N., Ahmed, Zeeshan, Akrami, Yashar, Anderson, Adam J., Ansarinejad, Behzad, Austermann, Jason, Baccigalupi, Carlo, Barkats, Denis, Barron, Darcy, Barry, Peter S., Battaglia, Nicholas, Baxter, Eric, Beck, Dominic, Bender, Amy N., Bennett, Charles, Beringue, Benjamin, Bischoff, Colin, Bleem, Lindsey, Bock, James, Bolliet, Boris, Bond, J Richard, Borrill, Julian, Brinckmann, Thejs, Brown, Michael L., Calabrese, Erminia, Carlstrom, John, Challinor, Anthony, Chang, Chihway, Chinone, Yuji, Clark, Susan E., Coulton, William, Cukierman, Ari, Cyr-Racine, Francis-Yan, Duff, Shannon M., Dvorkin, Cora, van Engelen, Alexander, Errard, Josquin, Eskilt, Johannes R., Essinger-Hileman, Thomas, Fabbian, Giulio, Feng, Chang, Ferraro, Simone, Filippini, Jeffrey, Freese, Katherine, Galitzki, Nicholas, Gawiser, Eric, Grin, Daniel, Grohs, Evan, Gruppuso, Alessandro, Gudmundsson, Jon E., Halverson, Nils W., Hamilton, Jean-Christophe, Harrington, Kathleen, Henrot-Versillé, Sophie, Hensley, Brandon, Hill, J. Colin, Hincks, Adam D., Hlozek, Renee, Holzapfel, William, Hotinli, Selim C., Hui, Howard, Ibitoye, Ayodeji, Johnson, Matthew, Johnson, Bradley R., Kang, Jae Hwan, Karkare, Kirit S., Knox, Lloyd, Kovac, John, Lau, Kenny, Legrand, Louis, Loverde, Marilena, Lubin, Philip, Ma, Yin-Zhe, Mroczkowski, Tony, Mukherjee, Suvodip, Münchmeyer, Moritz, Nagai, Daisuke, Nagy, Johanna, Niemack, Michael, Novosad, Valentine, Omori, Yuuki, Orlando, Giorgio, Pan, Zhaodi, Perotto, Laurence, Petroff, Matthew A., Pogosian, Levon, Pryke, Clem, Rahlin, Alexandra, Raveri, Marco, Reichardt, Christian L., Remazeilles, Mathieu, Rephaeli, Yoel, Ruhl, John, Schaan, Emmanuel, Shandera, Sarah, Shimon, Meir, Soliman, Ahmed, Stark, Antony A., Starkman, Glenn D., Stompor, Radek, Thakur, Ritoban Basu, Trendafilova, Cynthia, Tristram, Matthieu, Trivedi, Pranjal, Tucker, Gregory, Di Valentino, Eleonora, Vieira, Joaquin, Vieregg, Abigail, Wang, Gensheng, Watson, Scott, Wenzl, Lukas, Wollack, Edward J., Wu, W. L. Kimmy, Xu, Zhilei, Zegeye, David, and Zhang, Cheng
Abstract: This is a solicited whitepaper for the Snowmass 2021 community planning exercise. The paper focuses on measurements and science with the Cosmic Microwave Background (CMB). The CMB is foundational to our understanding of modern physics and continues to be a powerful tool driving our understanding of cosmology and particle physics. In this paper, we outline the broad and unique impact of CMB science for the High Energy Cosmic Frontier in the upcoming decade. We also describe the progression of ground-based CMB experiments, which shows that the community is prepared to develop the key capabilities and facilities needed to achieve these transformative CMB measurements., Comment: contribution to Snowmass 2021
Published: 2022

13. An exploration of an early gravity transition in light of cosmological tensions

Author: Benevento, Giampaolo, Kable, Joshua A., Addison, Graeme E., Bennett, Charles L., Benevento, Giampaolo, Kable, Joshua A., Addison, Graeme E., and Bennett, Charles L.
Abstract: We study a step-like transition in the value of the effective Planck mass (or effective gravitational constant) on cosmological scales prior to recombination. We employ CMB, BAO, and SNIa data and find they are sufficient to strongly constrain our implementation of the Effective Field Theory of Dark Energy and Modified Gravity, used to model the transition, to a limited parameter space. The data prefer a $\sim 5\%$ shift in the value of the effective Planck mass ($<10 \%$ at $2 \sigma$) prior to recombination. This Transitional Planck Mass (TPM) model is free to undergo its transition at any point over multiple decades of scale factor prior to recombination, $\log_{10}(a) = -5.32^{+0.96}_{-0.72}$ (68\% CL). This lowers the sound horizon at last scattering, which increases the Hubble constant to $71.09 \pm 0.75$ km $\textrm{s}^{-1}\textrm{Mpc}^{-1}$ with a combination of local measurements as prior and to $69.22^{+0.67}_{-0.86}$ km $\textrm{s}^{-1}\textrm{Mpc}^{-1}$ when the prior is excluded. The TPM model improves $\chi^2$ with respect to $\Lambda$CDM by $\Delta \chi^2 = -23.72$ with the $H_0$ prior and $\Delta \chi^2 = -4.8$ without the prior. The model allows for both $H_0 > 70$ km$\textrm{s}^{-1}\textrm{Mpc}^{-1}$ and $S_8 < 0.80$ simultaneously with lower values of $S_8$ due to a reduction in the matter density $\Omega_m$ to offset the increase in $H_0$ relative to $\Lambda$CDM. While this is a particular modified gravity model, studying other variants of modified gravity may be a productive path for potentially resolving cosmological tensions, while avoiding the need for a cosmological constant., Comment: 18 pages, 6 figures, 2 tables. Submitted to ApJ
Published: 2022

14. Construction of a Large Diameter Reflective Half-Wave Plate Modulator for Millimeter Wave Applications

Author: Eimer, Joseph R., Brewer, Michael K., Chuss, David T., Karakla, John, Shi, Rui, Appel, John W., Bennett, Charles L., Cleary, Joseph, Dahal, Sumit, Datta, Rahul, Essinger-Hileman, Thomas, Marriage, Tobias A., Núñez, Carolina, Petroff, Matthew A., Watts, Duncan J., Wollack, Edward J., Xu, Zhilei, Eimer, Joseph R., Brewer, Michael K., Chuss, David T., Karakla, John, Shi, Rui, Appel, John W., Bennett, Charles L., Cleary, Joseph, Dahal, Sumit, Datta, Rahul, Essinger-Hileman, Thomas, Marriage, Tobias A., Núñez, Carolina, Petroff, Matthew A., Watts, Duncan J., Wollack, Edward J., and Xu, Zhilei
Abstract: Polarization modulation is a powerful technique to increase the stability of measurements by enabling the distinction of a polarized signal from dominant slow system drifts and unpolarized foregrounds. Furthermore, when placed as close to the sky as possible, modulation can reduce systematic errors from instrument polarization. In this work, we introduce the design and preliminary drive system laboratory performance of a new 60 cm diameter reflective half-wave plate (RHWP) polarization modulator. The wave plate consists of a wire array situated in front of a flat mirror. Using \mbox{50 $\mu$m} diameter wires with \mbox{175 $\mu$m} spacing, the wave plate will be suitable for operation in the millimeter wavelength range with flatness of the wires and parallelism to the mirror held to a small fraction of a wavelength. The presented design targets the 77--108 GHz range. Modulation is performed by a rotation of the wave plate with a custom rotary drive utilizing an actively controlled servo motor., Comment: 13 pages, 7 figures, to appear in Proc. SPIE Astronomical Telescopes and Instrumentation 2022
Published: 2022

15. Characterization of aerogel scattering filters for astronomical telescopes

Author: Barlis, Alyssa, Arseneau, Stefan, Bennett, Charles L., Essinger-Hileman, Thomas, Guo, Haiquan, Helson, Kyle R., Marriage, Tobias, Quijada, Manuel A., Tokarz, Ariel E., Vivod, Stephanie L., Wollack, Edward J., Barlis, Alyssa, Arseneau, Stefan, Bennett, Charles L., Essinger-Hileman, Thomas, Guo, Haiquan, Helson, Kyle R., Marriage, Tobias, Quijada, Manuel A., Tokarz, Ariel E., Vivod, Stephanie L., and Wollack, Edward J.
Abstract: We have developed a suite of novel infrared-blocking filters made by embedding scattering particles in a polymer aerogel substrate. Our developments allow us to tune the spectral performance of the filters based on both the composition of the base aerogel material and the properties of the scattering particles. Our filters are targeted for use in a variety of applications, from ground-based CMB experiments to planetary science probes. We summarize the formulations we have fabricated and tested to date, including several polyimide base aerogel formulations incorporating a range of size distributions of diamond scattering particles. We also describe the spectral characterization techniques used to measure the filters' optical properties, including the development of a mm-wave Fourier transform spectrometer testbed., Comment: Presented at SPIE Astronomical Telescopes & Instrumentation Conference 2022
Published: 2022

16. Long-Timescale Stability in CMB Observations at Multiple Frequencies using Front-End Polarization Modulation

Author: Cleary, Joseph, Datta, Rahul, Appel, John W., Bennett, Charles L., Chuss, David T., Couto, Jullianna Denes, Dahal, Sumit, Espinoza, Francisco, Essinger-Hileman, Thomas, Harrington, Kathleen, Iuliano, Jeffrey, Li, Yunyang, Marriage, Tobias A., Nunez, Carolina, Petroff, Matthew A., Reeves, Rodrigo A., Shi, Rui, Watts, Duncan J., Wollack, Edward J., Xu, Zhilei, Cleary, Joseph, Datta, Rahul, Appel, John W., Bennett, Charles L., Chuss, David T., Couto, Jullianna Denes, Dahal, Sumit, Espinoza, Francisco, Essinger-Hileman, Thomas, Harrington, Kathleen, Iuliano, Jeffrey, Li, Yunyang, Marriage, Tobias A., Nunez, Carolina, Petroff, Matthew A., Reeves, Rodrigo A., Shi, Rui, Watts, Duncan J., Wollack, Edward J., and Xu, Zhilei
Abstract: The Cosmology Large Angular Scale Surveyor (CLASS) is a telescope array observing the Cosmic Microwave Background (CMB) at frequency bands centered near 40, 90, 150, and 220 GHz. CLASS measures the CMB polarization on the largest angular scales to constrain the inflationary tensor-to-scalar ratio and the optical depth due to reionization. To achieve the long time-scale stability necessary for this measurement from the ground, CLASS utilizes a front-end, variable-delay polarization modulator on each telescope. Here we report on the improvements in stability afforded by front-end modulation using data across all four CLASS frequencies. Across one month of modulated linear polarization data in 2021, CLASS achieved median knee frequencies of 9.1, 29.1, 20.4, and 36.4 mHz for the 40, 90, 150, and 220 GHz observing bands. The knee frequencies are approximately an order of magnitude lower than achieved via CLASS pair-differencing orthogonal detector pairs without modulation., Comment: Submitted to SPIE Astronomical Telescopes + Instrumentation 2022 Conference (AS22)
Published: 2022

17. Novel infrared-blocking aerogel scattering filters and their applications in astrophysical and planetary science

Author: Helson, Kyle R., Arseneau, Stefan, Barlis, Alyssa, Bennett, Charles L., Essinger-Hileman, Thomas M., Guo, Haiquan, Marriage, Tobias, Quijada, Manuel A., Tokarz, Ariel E., Vivod, Stephanie L., Wollack, Edward J., Helson, Kyle R., Arseneau, Stefan, Barlis, Alyssa, Bennett, Charles L., Essinger-Hileman, Thomas M., Guo, Haiquan, Marriage, Tobias, Quijada, Manuel A., Tokarz, Ariel E., Vivod, Stephanie L., and Wollack, Edward J.
Abstract: Infrared-blocking scattering aerogel filters have a broad range of potential applications in astrophysics and planetary science observations in the far-infrared, sub-millimeter, and microwave regimes. Successful dielectric modeling of aerogel filters allowed the fabrication of samples to meet the mechanical and science instrument requirements for several experiments, including the Sub-millimeter Solar Observation Lunar Volatiles Experiment (SSOLVE), the Cosmology Large Angular Scale Surveyor (CLASS), and the Experiment for Cryogenic Large-Aperture Intensity Mapping (EXCLAIM). Thermal multi-physics simulations of the filters predict their performance when integrated into a cryogenic receiver. Prototype filters have survived cryogenic cycling to 4K with no degradation in mechanical properties.
Published: 2022

18. Design and characterization of new 90 GHz detectors for the Cosmology Large Angular Scale Surveyor (CLASS)

Author: Núñez, Carolina, Appel, John W., Bruno, Sarah Marie, Datta, Rahul, Ali, Aamir, Bennett, Charles L., Dahal, Sumit, Couto, Jullianna Denes, Denis, Kevin L., Eimer, Joseph, Espinoza, Francisco, Essinger-Hileman, Tom, Helson, Kyle, Iuliano, Jeffrey, Marriage, Tobias A., Pérez, Carolina Morales, Valle, Deniz Augusto Nunes, Petroff, Matthew A., Rostem, Karwan, Shi, Rui, Watts, Duncan J., Wollack, Edward J., Xu, Zhilei, Núñez, Carolina, Appel, John W., Bruno, Sarah Marie, Datta, Rahul, Ali, Aamir, Bennett, Charles L., Dahal, Sumit, Couto, Jullianna Denes, Denis, Kevin L., Eimer, Joseph, Espinoza, Francisco, Essinger-Hileman, Tom, Helson, Kyle, Iuliano, Jeffrey, Marriage, Tobias A., Pérez, Carolina Morales, Valle, Deniz Augusto Nunes, Petroff, Matthew A., Rostem, Karwan, Shi, Rui, Watts, Duncan J., Wollack, Edward J., and Xu, Zhilei
Abstract: The Cosmology Large Angular Scale Surveyor (CLASS) is a polarization-sensitive telescope array located at an altitude of 5,200 m in the Chilean Atacama Desert. CLASS is designed to measure "E-mode" (even parity) and "B-mode" (odd parity) polarization patterns in the Cosmic Microwave Background (CMB) over large angular scales with the aim of improving our understanding of inflation, reionization, and dark matter. CLASS is currently observing with three telescopes covering four frequency bands: one at 40 GHz (Q); one at 90 GHz (W1); and one dichroic system at 150/220 GHz (G). In these proceedings, we discuss the updated design and in-lab characterization of new 90 GHz detectors. The new detectors include design changes to the transition-edge sensor (TES) bolometer architecture, which aim to improve stability and optical efficiency. We assembled and tested four new detector wafers, to replace four modules of the W1 focal plane. These detectors were installed into the W1 telescope, and will achieve first light in the austral winter of 2022. We present electrothermal parameters and bandpass measurements from in-lab dark and optical testing. From in-lab dark tests, we also measure a median NEP of 12.3 $\mathrm{aW\sqrt{s}}$ across all four wafers about the CLASS signal band, which is below the expected photon NEP of 32 $\mathrm{aW\sqrt{s}}$ from the field. We therefore expect the new detectors to be photon noise limited., Comment: 10 pages, 6 figures, to appear in Proc. SPIE Astronomical Telescopes and Instrumentation 2022
Published: 2022

19. Testing CMB Anomalies in E-mode Polarization with Current and Future Data

Author: Shi, Rui, Marriage, Tobias A., Appel, John W., Bennett, Charles L., Chuss, David T., Cleary, Joseph, Eimer, Joseph, Dahal, Sumit, Datta, Rahul, Espinoza, Francisco, Li, Yunyang, Miller, Nathan J., Núñez, Carolina, Padilla, Ivan L., Petroff, Matthew A., Valle, Deniz A. N., Wollack, Edward J., Xu, Zhilei, Shi, Rui, Marriage, Tobias A., Appel, John W., Bennett, Charles L., Chuss, David T., Cleary, Joseph, Eimer, Joseph, Dahal, Sumit, Datta, Rahul, Espinoza, Francisco, Li, Yunyang, Miller, Nathan J., Núñez, Carolina, Padilla, Ivan L., Petroff, Matthew A., Valle, Deniz A. N., Wollack, Edward J., and Xu, Zhilei
Abstract: In this paper, we explore the power of the cosmic microwave background (CMB) polarization (E-mode) data to corroborate four potential anomalies in CMB temperature data: the lack of large angular-scale correlations, the alignment of the quadrupole and octupole (Q-O), the point-parity asymmetry, and the hemispherical power asymmetry. We use CMB simulations with noise representative of three experiments -- the Planck satellite, the Cosmology Large Angular Scale Surveyor (CLASS), and the LiteBIRD satellite -- to test how current and future data constrain the anomalies. We find the correlation coefficients $\rho$ between temperature and E-mode estimators to be less than $0.1$, except for the point-parity asymmetry ($\rho=0.17$ for cosmic-variance-limited simulations), confirming that E-modes provide a check on the anomalies that is largely independent of temperature data. Compared to Planck component-separated CMB data (SMICA), the putative LiteBIRD survey would reduce errors on E-mode anomaly estimators by factors of $\sim 3$ for hemispherical power asymmetry and point-parity asymmetry, and by $\sim 26$ for lack of large-scale correlation. The improvement in Q-O alignment is not obvious due to large cosmic variance, but we found the ability to pin down the estimator value will be improved by a factor $\gtrsim100$. Improvements with CLASS are intermediate to these., Comment: 23 pages, 15 figures, 6 tables. Published in ApJ
Published: 2022
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20. Calibration of Transition-edge Sensor (TES) Bolometer Arrays with Application to CLASS

Author: Appel, John W., Bennett, Charles L., Brewer, Michael K., Bustos, Ricardo, Chan, Manwei, Chuss, David T., Cleary, Joseph, Couto, Jullianna D., Dahal, Sumit, Datta, Rahul, Denis, Kevin, Eimer, Joseph, Essinger-Hileman, Thomas, Harrington, Kathleen, Iuliano, Jeffrey, Li, Yunyang, Marriage, Tobias A., Núñez, Carolina, Osumi, Keisuke, Padilla, Ivan L., Petroff, Matthew A., Rostem, Karwan, Valle, Deniz A. N., Watts, Duncan J., Weiland, Janet L., Wollack, Edward J., Xu, Zhilei, Appel, John W., Bennett, Charles L., Brewer, Michael K., Bustos, Ricardo, Chan, Manwei, Chuss, David T., Cleary, Joseph, Couto, Jullianna D., Dahal, Sumit, Datta, Rahul, Denis, Kevin, Eimer, Joseph, Essinger-Hileman, Thomas, Harrington, Kathleen, Iuliano, Jeffrey, Li, Yunyang, Marriage, Tobias A., Núñez, Carolina, Osumi, Keisuke, Padilla, Ivan L., Petroff, Matthew A., Rostem, Karwan, Valle, Deniz A. N., Watts, Duncan J., Weiland, Janet L., Wollack, Edward J., and Xu, Zhilei
Abstract: The current and future cosmic microwave background (CMB) experiments fielding kilo-pixel arrays of transition-edge sensor (TES) bolometers require accurate and robust gain calibration methods. We simplify and refactor the standard TES model to directly relate the detector responsivity calibration and optical time constant to the measured TES current $I$ and the applied bias current $I_{\mathrm{b}}$. The calibration method developed for the Cosmology Large Angular Scale Surveyor (CLASS) TES bolometer arrays relies on current versus voltage ($I$-$V$) measurements acquired daily prior to CMB observations. By binning Q-band (40GHz) $I$-$V$ measurements by optical loading, we find that the gain calibration median standard error within a bin is 0.3%. We test the accuracy of this "$I$-$V$ bin" detector calibration method by using the Moon as a photometric standard. The ratio of measured Moon amplitudes between detector pairs sharing the same feedhorn indicates a TES calibration error of 0.5%. We also find that for the CLASS Q-band TES array, calibrating the response of individual detectors based solely on the applied TES bias current accurately corrects TES gain variations across time but introduces a bias in the TES calibration from data counts to power units. Since the TES current bias value is set and recorded before every observation, this calibration method can always be applied to raw TES data and is not subject to $I$-$V$ data quality or processing errors., Comment: 19 pages, 7 figures, 5 tables. Submitted to ApJS May 2022. Published ApJS Oct 2022
Published: 2022
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21. Four-year Cosmology Large Angular Scale Surveyor (CLASS) Observations: On-sky Receiver Performance at 40, 90, 150, and 220 GHz Frequency Bands

Author: Dahal, Sumit, Appel, John W., Datta, Rahul, Brewer, Michael K., Ali, Aamir, Bennett, Charles L., Bustos, Ricardo, Chan, Manwei, Chuss, David T., Cleary, Joseph, Couto, Jullianna D., Denis, Kevin L., Dünner, Rolando, Eimer, Joseph, Espinoza, Francisco, Essinger-Hileman, Thomas, Golec, Joseph E., Harrington, Kathleen, Helson, Kyle, Iuliano, Jeffrey, Karakla, John, Li, Yunyang, Marriage, Tobias A., McMahon, Jeffrey J., Miller, Nathan J., Novack, Sasha, Núñez, Carolina, Osumi, Keisuke, Padilla, Ivan L., Palma, Gonzalo A., Parker, Lucas, Petroff, Matthew A., Reeves, Rodrigo, Rhoades, Gary, Rostem, Karwan, Valle, Deniz A. N., Watts, Duncan J., Weiland, Janet L., Wollack, Edward J., Xu, Zhilei, Dahal, Sumit, Appel, John W., Datta, Rahul, Brewer, Michael K., Ali, Aamir, Bennett, Charles L., Bustos, Ricardo, Chan, Manwei, Chuss, David T., Cleary, Joseph, Couto, Jullianna D., Denis, Kevin L., Dünner, Rolando, Eimer, Joseph, Espinoza, Francisco, Essinger-Hileman, Thomas, Golec, Joseph E., Harrington, Kathleen, Helson, Kyle, Iuliano, Jeffrey, Karakla, John, Li, Yunyang, Marriage, Tobias A., McMahon, Jeffrey J., Miller, Nathan J., Novack, Sasha, Núñez, Carolina, Osumi, Keisuke, Padilla, Ivan L., Palma, Gonzalo A., Parker, Lucas, Petroff, Matthew A., Reeves, Rodrigo, Rhoades, Gary, Rostem, Karwan, Valle, Deniz A. N., Watts, Duncan J., Weiland, Janet L., Wollack, Edward J., and Xu, Zhilei
Abstract: The Cosmology Large Angular Scale Surveyor (CLASS) observes the polarized cosmic microwave background (CMB) over the angular scales of 1$^\circ \lesssim \theta \leq$ 90$^\circ$ with the aim of characterizing primordial gravitational waves and cosmic reionization. We report on the on-sky performance of the CLASS Q-band (40 GHz), W-band (90 GHz), and dichroic G-band (150/220 GHz) receivers that have been operational at the CLASS site in the Atacama desert since June 2016, May 2018, and September 2019, respectively. We show that the noise-equivalent power measured by the detectors matches the expected noise model based on on-sky optical loading and lab-measured detector parameters. Using Moon, Venus, and Jupiter observations, we obtain power-to-antenna-temperature calibrations and optical efficiencies for the telescopes. From the CMB survey data, we compute instantaneous array noise-equivalent-temperature sensitivities of 22, 19, 23, and 71 $\mathrm{\mu K}_\mathrm{cmb}\sqrt{\mathrm{s}}$ for the 40, 90, 150, and 220 GHz frequency bands, respectively. These noise temperatures refer to white noise amplitudes, which contribute to sky maps at all angular scales. Future papers will assess additional noise sources impacting larger angular scales., Comment: 13 pages, 3 figures, published in ApJ
Published: 2021
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22. Limits on Polarized Dust Spectral Index Variations for CMB Foreground Analysis

Author: Osumi, Keisuke, Weiland, Janet L., Addison, Graeme E., Bennett, Charles L., Osumi, Keisuke, Weiland, Janet L., Addison, Graeme E., and Bennett, Charles L.
Abstract: Using Planck polarization data, we search for and constrain spatial variations of the polarized dust foreground for cosmic microwave background (CMB) observations, specifically in its spectral index, $\beta_d$. Failure to account for such variations will cause errors in the foreground cleaning that propagate into errors on cosmological parameter recovery from the cleaned CMB map. It is unclear how robust prior studies of the Planck data which constrained $\beta_d$ variations are due to challenges with noise modeling, residual systematics, and priors. To clarify constraints on $\beta_d$ and its variation, we employ two pixel space analyses of the polarized dust foreground at $>3.7^{\circ}$ scales on $\approx 60\%$ of the sky at high Galactic latitudes. A template fitting method, which measures $\beta_d$ over three regions of $\approx 20\%$ of the sky, does not find significant deviations from an uniform $\beta_d = 1.55$, consistent with prior Planck determinations. An additional analysis in these regions, based on multifrequency fits to a dust and CMB model per pixel, puts limits on $\sigma_{\beta_d}$, the Gaussian spatial variation in $\beta_d$. At the highest latitudes, the data support $\sigma_{\beta_d}$ up to $0.45$, $0.30$ at mid-latitudes, and $0.15$ at low-latitudes. We also demonstrate that care must be taken when interpreting the current Planck constraints, $\beta_d$ maps, and noise simulations. Due to residual systematics and low dust signal to noise at high latitudes, forecasts for ongoing and future missions should include the possibility of large values of $\sigma_{\beta_d}$ as estimated in this paper, based on current polarization data., Comment: 17 pages, 10 figures, 4 tables, version accepted by ApJ
Published: 2021
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23. Consequences to patients, clinicians, and manufacturers when very serious adverse drug reactions are identified (1997–2019):A qualitative analysis from the Southern Network on Adverse Reactions (SONAR)

Author: Bennett, Charles L., Hoque, Shamia, Olivieri, Nancy, Taylor, Matthew A., Aboulafia, David, Lubaczewski, Courtney, Bennett, Andrew C., Vemula, Jay, Schooley, Benjamin, Witherspoon, Bartlett J., Godwin, Ashley C., Ray, Paul S., Yarnold, Paul R., Ausdenmoore, Henry C., Fishman, Marc, Herring, Georgne, Ventrone, Anne, Aldaco, Juan, Hrushesky, William J., Restaino, John, Thomsen, Henrik S., Marx, Robert, Migliorati, Cesar, Ruggiero, Salvatore, Nabhan, Chadi, Carson, Kenneth R., McKoy, June M., Yang, Y. Tony, Schoen, Martin W., Knopf, Kevin, Martin, Linda, Sartor, Oliver, Rosen, Steven, Smith, William K., Bennett, Charles L., Hoque, Shamia, Olivieri, Nancy, Taylor, Matthew A., Aboulafia, David, Lubaczewski, Courtney, Bennett, Andrew C., Vemula, Jay, Schooley, Benjamin, Witherspoon, Bartlett J., Godwin, Ashley C., Ray, Paul S., Yarnold, Paul R., Ausdenmoore, Henry C., Fishman, Marc, Herring, Georgne, Ventrone, Anne, Aldaco, Juan, Hrushesky, William J., Restaino, John, Thomsen, Henrik S., Marx, Robert, Migliorati, Cesar, Ruggiero, Salvatore, Nabhan, Chadi, Carson, Kenneth R., McKoy, June M., Yang, Y. Tony, Schoen, Martin W., Knopf, Kevin, Martin, Linda, Sartor, Oliver, Rosen, Steven, and Smith, William K.
Abstract: Background: Adverse drug/device reactions (ADRs) can result in severe patient harm. We define very serious ADRs as being associated with severe toxicity, as measured on the Common Toxicity Criteria Adverse Events (CTCAE)) scale, following use of drugs or devices with large sales, large financial settlements, and large numbers of injured persons. We report on impacts on patients, clinicians, and manufacturers following very serious ADR reporting. Methods: We reviewed clinician identified very serious ADRs published between 1997 and 2019. Drugs and devices associated with reports of very serious ADRs were identified. Included drugs or devices had market removal discussed at Food and Drug Advisory (FDA) Advisory Committee meetings, were published by clinicians, had sales > $1 billion, were associated with CTCAE Grade 4 or 5 toxicity effects, and had either >$1 billion in settlements or >1,000 injured patients. Data sources included journals, Congressional transcripts, and news reports. We reviewed data on: 1) timing of ADR reports, Boxed warnings, and product withdrawals, and 2) patient, clinician, and manufacturer impacts. Binomial analysis was used to compare sales pre- and post-FDA Advisory Committee meetings. Findings: Twenty very serious ADRs involved fifteen drugs and one device. Legal settlements totaled $38.4 billion for 753,900 injured persons. Eleven of 18 clinicians (61%) reported harms, including verbal threats from manufacturer (five) and loss of a faculty position (one). Annual sales decreased 94% from $29.1 billion pre-FDA meeting to $4.9 billion afterwards (p<0.0018). Manufacturers of four drugs paid $1.7 billion total in criminal fines for failing to inform the FDA and physicians about very serious ADRs. Following FDA approval, the median time to ADR reporting was 7.5 years (Interquartile range 3,13 years). Twelve drugs received Box warnings and one drug received a warning (median, 7.5 years following ADR reporting (IQR 5,11 years). Six
Published: 2021

24. Bennett, Charles

Author: Bennett, Charles and Bennett, Charles
Published: 2021

25. Pain

Author: Bennett, Charles G.
Subjects: 616
Published: 1892

26. Full-sky Cosmic Microwave Background Foreground Cleaning Using Machine Learning

Author: Petroff, Matthew A., Addison, Graeme E., Bennett, Charles L., Weiland, Janet L., Petroff, Matthew A., Addison, Graeme E., Bennett, Charles L., and Weiland, Janet L.
Abstract: In order to extract cosmological information from observations of the millimeter and submillimeter sky, foreground components must first be removed to produce an estimate of the cosmic microwave background (CMB). We developed a machine-learning approach for doing so for full-sky temperature maps of the millimeter and submillimeter sky. We constructed a Bayesian spherical convolutional neural network architecture to produce a model that captures both spectral and morphological aspects of the foregrounds. Additionally, the model outputs a per-pixel error estimate that incorporates both statistical and model uncertainties. The model was then trained using simulations that incorporated knowledge of these foreground components that was available at the time of the launch of the Planck satellite. On simulated maps, the CMB is recovered with a mean absolute difference of $<4\mu$K over the full sky after masking map pixels with a predicted standard error of $>50\mu$K; the angular power spectrum is also accurately recovered. Once validated with the simulations, this model was applied to Planck temperature observations from its 70GHz through 857GHz channels to produce a foreground-cleaned CMB map at a Healpix map resolution of NSIDE=512. Furthermore, we demonstrate the utility of the technique for evaluating how well different simulations match observations, particularly in regard to the modeling of thermal dust., Comment: 10 pages, 6 figures, submitted to ApJ
Published: 2020
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27. Two Year Cosmology Large Angular Scale Surveyor (CLASS) Observations: Long Timescale Stability Achieved with a Front-End Variable-delay Polarization Modulator at 40 GHz

Author: Harrington, Kathleen, Datta, Rahul, Osumi, Keisuke, Ali, Aamir, Appel, John W., Bennett, Charles L., Brewer, Michael K., Bustos, Ricardo, Chan, Manwei, Chuss, David T., Cleary, Joseph, Couto, Jullianna Denes, Dahal, Sumit, Dünner, Rolando, Eimer, Joseph R., Essinger-Hileman, Thomas, Hubmayr, Johannes, Inostroza, Francisco Raul Espinoza, Iuliano, Jeffrey, Karakla, John, Li, Yunyang, Marriage, Tobias A., Miller, Nathan J., Núñez, Carolina, Padilla, Ivan L., Parker, Lucas, Petroff, Matthew A., Márquez, Bastian Pradenas, Reeves, Rodrigo, Rojas, Pedro Fluxá, Rostem, Karwan, Valle, Deniz Augusto Nunes, Watts, Duncan J., Weiland, Janet L., Wollack, Edward J., Xu, Zhilei, Harrington, Kathleen, Datta, Rahul, Osumi, Keisuke, Ali, Aamir, Appel, John W., Bennett, Charles L., Brewer, Michael K., Bustos, Ricardo, Chan, Manwei, Chuss, David T., Cleary, Joseph, Couto, Jullianna Denes, Dahal, Sumit, Dünner, Rolando, Eimer, Joseph R., Essinger-Hileman, Thomas, Hubmayr, Johannes, Inostroza, Francisco Raul Espinoza, Iuliano, Jeffrey, Karakla, John, Li, Yunyang, Marriage, Tobias A., Miller, Nathan J., Núñez, Carolina, Padilla, Ivan L., Parker, Lucas, Petroff, Matthew A., Márquez, Bastian Pradenas, Reeves, Rodrigo, Rojas, Pedro Fluxá, Rostem, Karwan, Valle, Deniz Augusto Nunes, Watts, Duncan J., Weiland, Janet L., Wollack, Edward J., and Xu, Zhilei
Abstract: The Cosmology Large Angular Scale Surveyor (CLASS) is a four-telescope array observing the largest angular scales ($2 \lesssim \ell \lesssim 200$) of the cosmic microwave background (CMB) polarization. These scales encode information about reionization and inflation during the early universe. The instrument stability necessary to observe these angular scales from the ground is achieved through the use of a variable-delay polarization modulator (VPM) as the first optical element in each of the CLASS telescopes. Here we develop a demodulation scheme used to extract the polarization timestreams from the CLASS data and apply this method to selected data from the first two years of observations by the 40 GHz CLASS telescope. These timestreams are used to measure the $1/f$ noise and temperature-to-polarization ($T\rightarrow P$) leakage present in the CLASS data. We find a median knee frequency for the pair-differenced demodulated linear polarization of 15.12 mHz and a $T\rightarrow P$ leakage of $<3.8\times10^{-4}$ (95\% confidence) across the focal plane. We examine the sources of $1/f$ noise present in the data and find the component of $1/f$ due to atmospheric precipitable water vapor (PWV) has an amplitude of $203 \pm 12 \mathrm{\mu K_{RJ}\sqrt{s}}$ for 1 mm of PWV when evaluated at 10 mHz; accounting for $\sim32\%$ of the $1/f$ noise in the central pixels of the focal plane. The low level of $T\rightarrow P$ leakage and $1/f$ noise achieved through the use of a front-end polarization modulator enables the observation of the largest scales of the CMB polarization from the ground by the CLASS telescopes., Comment: Submitted to ApJ
Published: 2020
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28. Control and systems software for the Cosmology Large Angular Scale Surveyor (CLASS)

Author: Petroff, Matthew A., Appel, John W., Bennett, Charles L., Brewer, Michael K., Chan, Manwei, Chuss, David T., Cleary, Joseph, Couto, Jullianna Denes, Dahal, Sumit, Eimer, Joseph R., Essinger-Hileman, Thomas, Rojas, Pedro Fluxá, Harrington, Kathleen, Iuliano, Jeffrey, Marriage, Tobias A., Miller, Nathan J., Valle, Deniz Augusto Nunes, Watts, Duncan J., Xu, Zhilei, Petroff, Matthew A., Appel, John W., Bennett, Charles L., Brewer, Michael K., Chan, Manwei, Chuss, David T., Cleary, Joseph, Couto, Jullianna Denes, Dahal, Sumit, Eimer, Joseph R., Essinger-Hileman, Thomas, Rojas, Pedro Fluxá, Harrington, Kathleen, Iuliano, Jeffrey, Marriage, Tobias A., Miller, Nathan J., Valle, Deniz Augusto Nunes, Watts, Duncan J., and Xu, Zhilei
Abstract: The Cosmology Large Angular Scale Surveyor (CLASS) is an array of polarization-sensitive millimeter wave telescopes that observes ~70% of the sky at frequency bands centered near 40GHz, 90GHz, 150GHz, and 220GHz from the Atacama desert of northern Chile. Here, we describe the architecture of the software used to control the telescopes, acquire data from the various instruments, schedule observations, monitor the status of the instruments and observations, create archival data packages, and transfer data packages to North America for analysis. The computer and network architecture of the CLASS observing site is also briefly discussed. This software and architecture has been in use since 2016, operating the telescopes day and night throughout the year, and has proven successful in fulfilling its design goals., Comment: 19 pages, 8 figures, to appear in Proc. SPIE
Published: 2020
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29. Venus Observations at 40 and 90 GHz with CLASS

Author: Dahal, Sumit, Brewer, Michael K., Appel, John W., Ali, Aamir, Bennett, Charles L., Bustos, Ricardo, Chan, Manwei, Chuss, David T., Cleary, Joseph, Couto, Jullianna D., Datta, Rahul, Denis, Kevin L., Eimer, Joseph, Espinoza, Francisco, Essinger-Hileman, Thomas, Gothe, Dominik, Harrington, Kathleen, Iuliano, Jeffrey, Karakla, John, Marriage, Tobias A., Novack, Sasha, Núñez, Carolina, Padilla, Ivan L., Parker, Lucas, Petroff, Matthew A., Reeves, Rodrigo, Rhoades, Gary, Rostem, Karwan, Valle, Deniz A. N., Watts, Duncan J., Weiland, Janet L., Wollack, Edward J., Xu, Zhilei, Dahal, Sumit, Brewer, Michael K., Appel, John W., Ali, Aamir, Bennett, Charles L., Bustos, Ricardo, Chan, Manwei, Chuss, David T., Cleary, Joseph, Couto, Jullianna D., Datta, Rahul, Denis, Kevin L., Eimer, Joseph, Espinoza, Francisco, Essinger-Hileman, Thomas, Gothe, Dominik, Harrington, Kathleen, Iuliano, Jeffrey, Karakla, John, Marriage, Tobias A., Novack, Sasha, Núñez, Carolina, Padilla, Ivan L., Parker, Lucas, Petroff, Matthew A., Reeves, Rodrigo, Rhoades, Gary, Rostem, Karwan, Valle, Deniz A. N., Watts, Duncan J., Weiland, Janet L., Wollack, Edward J., and Xu, Zhilei
Abstract: Using the Cosmology Large Angular Scale Surveyor, we measure the disk-averaged absolute Venus brightness temperature to be 432.3 $\pm$ 2.8 K and 355.6 $\pm$ 1.3 K in the Q and W frequency bands centered at 38.8 and 93.7 GHz, respectively. At both frequency bands, these are the most precise measurements to date. Furthermore, we observe no phase dependence of the measured temperature in either band. Our measurements are consistent with a CO$_2$-dominant atmospheric model that includes trace amounts of additional absorbers like SO$_2$ and H$_2$SO$_4$., Comment: 7 pages, 3 figures, published in PSJ
Published: 2020
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30. Deconstructing the Planck TT Power Spectrum to Constrain Deviations from $\Lambda$CDM

Author: Kable, Joshua A., Addison, Graeme E., Bennett, Charles L., Kable, Joshua A., Addison, Graeme E., and Bennett, Charles L.
Abstract: Consistency checks of $\Lambda$CDM predictions with current cosmological data sets may illuminate the types of changes needed to resolve cosmological tensions. To this end, we modify the CLASS Boltzmann code to create phenomenological amplitudes, similar to the lensing amplitude parameter $A_L$, for the Sachs-Wolfe, Doppler, early Integrated Sachs-Wolfe (eISW), and Polarization contributions to the CMB temperature anisotropy, and then we include these additional amplitudes in fits to the Planck TT power spectrum. We find that allowing one of these amplitudes to vary at a time results in little improvement over $\Lambda$CDM alone suggesting that each of these physical effects are being correctly accounted for given the current level of precision. Further, we find that the only pair of phenomenological amplitudes that results in a significant improvement to the fit to Planck temperature data results from varying the amplitudes of the Sachs-Wolfe and Doppler effects simultaneously. However, we show that this model is really just refinding the $\Lambda$CDM + $A_L$ solution. We test adding our phenomenological amplitudes as well as $N_{\textrm{eff}}$, $Y_{\textrm{He}}$, and $n_{\textrm{run}}$ to $\Lambda$CDM + $A_L$ and find that none of these model extensions provide significant improvement over $\Lambda$CDM + $A_L$ when fitting Planck temperature data. Finally, we quantify the contributions of both the eISW effect and lensing on the constraint of the physical matter density from Planck temperature data by allowing the phenomenological amplitude from each effect to vary. We find that these effects play a relatively small role (the uncertainty increases by $3.5\%$ and $16\%$ respectively) suggesting that the overall photon envelope has the greatest constraining power., Comment: 17 pages, 6 figures, Published by ApJ
Published: 2020
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31. Dark Matter Science in the Era of LSST

Author: Bechtol, Keith, Bechtol, Keith, Drlica-Wagner, Alex, Abazajian, Kevork N, Abidi, Muntazir, Adhikari, Susmita, Ali-Haïmoud, Yacine, Annis, James, Ansarinejad, Behzad, Armstrong, Robert, Asorey, Jacobo, Baccigalupi, Carlo, Banerjee, Arka, Banik, Nilanjan, Bennett, Charles, Beutler, Florian, Bird, Simeon, Birrer, Simon, Biswas, Rahul, Biviano, Andrea, Blazek, Jonathan, Boddy, Kimberly K, Bonaca, Ana, Borrill, Julian, Bose, Sownak, Bovy, Jo, Frye, Brenda, Brooks, Alyson M, Buckley, Matthew R, Buckley-Geer, Elizabeth, Bulbul, Esra, Burchat, Patricia R, Burgess, Cliff, Calore, Francesca, Caputo, Regina, Castorina, Emanuele, Chang, Chihway, Chapline, George, Charles, Eric, Chen, Xingang, Clowe, Douglas, Cohen-Tanugi, Johann, Comparat, Johan, Croft, Rupert AC, Cuoco, Alessandro, Cyr-Racine, Francis-Yan, D'Amico, Guido, Davis, Tamara M, Dawson, William A, Macorra, Axel de la, Valentino, Eleonora Di, Rivero, Ana Díaz, Digel, Seth, Dodelson, Scott, Doré, Olivier, Dvorkin, Cora, Eckner, Christopher, Ellison, John, Erkal, Denis, Farahi, Arya, Fassnacht, Christopher D, Ferreira, Pedro G, Flaugher, Brenna, Foreman, Simon, Friedrich, Oliver, Frieman, Joshua, García-Bellido, Juan, Gawiser, Eric, Gerbino, Martina, Giannotti, Maurizio, Gill, Mandeep SS, Gluscevic, Vera, Golovich, Nathan, Gontcho, Satya Gontcho A, González-Morales, Alma X, Grin, Daniel, Gruen, Daniel, Hearin, Andrew P, Hendel, David, Hezaveh, Yashar D, Hirata, Christopher M, Hložek, Renee, Horiuchi, Shunsaku, Jain, Bhuvnesh, Jee, M James, Jeltema, Tesla E, Kamionkowski, Marc, Kaplinghat, Manoj, Keeley, Ryan E, Keeton, Charles R, Khatri, Rishi, Koposov, Sergey E, Koushiappas, Savvas M, Kovetz, Ely D, Lahav, Ofer, Lam, Casey, Lee, Chien-Hsiu, Li, Ting S, Liguori, Michele, Lin, Tongyan, Lisanti, Mariangela, Bechtol, Keith, Bechtol, Keith, Drlica-Wagner, Alex, Abazajian, Kevork N, Abidi, Muntazir, Adhikari, Susmita, Ali-Haïmoud, Yacine, Annis, James, Ansarinejad, Behzad, Armstrong, Robert, Asorey, Jacobo, Baccigalupi, Carlo, Banerjee, Arka, Banik, Nilanjan, Bennett, Charles, Beutler, Florian, Bird, Simeon, Birrer, Simon, Biswas, Rahul, Biviano, Andrea, Blazek, Jonathan, Boddy, Kimberly K, Bonaca, Ana, Borrill, Julian, Bose, Sownak, Bovy, Jo, Frye, Brenda, Brooks, Alyson M, Buckley, Matthew R, Buckley-Geer, Elizabeth, Bulbul, Esra, Burchat, Patricia R, Burgess, Cliff, Calore, Francesca, Caputo, Regina, Castorina, Emanuele, Chang, Chihway, Chapline, George, Charles, Eric, Chen, Xingang, Clowe, Douglas, Cohen-Tanugi, Johann, Comparat, Johan, Croft, Rupert AC, Cuoco, Alessandro, Cyr-Racine, Francis-Yan, D'Amico, Guido, Davis, Tamara M, Dawson, William A, Macorra, Axel de la, Valentino, Eleonora Di, Rivero, Ana Díaz, Digel, Seth, Dodelson, Scott, Doré, Olivier, Dvorkin, Cora, Eckner, Christopher, Ellison, John, Erkal, Denis, Farahi, Arya, Fassnacht, Christopher D, Ferreira, Pedro G, Flaugher, Brenna, Foreman, Simon, Friedrich, Oliver, Frieman, Joshua, García-Bellido, Juan, Gawiser, Eric, Gerbino, Martina, Giannotti, Maurizio, Gill, Mandeep SS, Gluscevic, Vera, Golovich, Nathan, Gontcho, Satya Gontcho A, González-Morales, Alma X, Grin, Daniel, Gruen, Daniel, Hearin, Andrew P, Hendel, David, Hezaveh, Yashar D, Hirata, Christopher M, Hložek, Renee, Horiuchi, Shunsaku, Jain, Bhuvnesh, Jee, M James, Jeltema, Tesla E, Kamionkowski, Marc, Kaplinghat, Manoj, Keeley, Ryan E, Keeton, Charles R, Khatri, Rishi, Koposov, Sergey E, Koushiappas, Savvas M, Kovetz, Ely D, Lahav, Ofer, Lam, Casey, Lee, Chien-Hsiu, Li, Ting S, Liguori, Michele, Lin, Tongyan, and Lisanti, Mariangela
Abstract: Astrophysical observations currently provide the only robust, empirical measurements of dark matter. In the coming decade, astrophysical observations will guide other experimental efforts, while simultaneously probing unique regions of dark matter parameter space. This white paper summarizes astrophysical observations that can constrain the fundamental physics of dark matter in the era of LSST. We describe how astrophysical observations will inform our understanding of the fundamental properties of dark matter, such as particle mass, self-interaction strength, non-gravitational interactions with the Standard Model, and compact object abundances. Additionally, we highlight theoretical work and experimental/observational facilities that will complement LSST to strengthen our understanding of the fundamental characteristics of dark matter.
Published: 2019

32. Messengers from the Early Universe: Cosmic Neutrinos and Other Light Relics

Author: Green, Daniel, Green, Daniel, Amin, Mustafa A, Meyers, Joel, Wallisch, Benjamin, Abazajian, Kevork N, Abidi, Muntazir, Adshead, Peter, Ahmed, Zeeshan, Ansarinejad, Behzad, Armstrong, Robert, Baccigalupi, Carlo, Bandura, Kevin, Barron, Darcy, Battaglia, Nicholas, Baumann, Daniel, Bechtol, Keith, Bennett, Charles, Benson, Bradford, Beutler, Florian, Bischoff, Colin, Bleem, Lindsey, Bond, J Richard, Borrill, Julian, Buckley-Geer, Elizabeth, Burgess, Cliff, Carlstrom, John E, Castorina, Emanuele, Challinor, Anthony, Chen, Xingang, Cooray, Asantha, Coulton, William, Craig, Nathaniel, Crawford, Thomas, Cyr-Racine, Francis-Yan, D'Amico, Guido, Demarteau, Marcel, Doré, Olivier, Yutong, Duan, Dunkley, Joanna, Dvorkin, Cora, Ellison, John, Engelen, Alexander van, Escoffier, Stephanie, Essinger-Hileman, Tom, Fabbian, Giulio, Filippini, Jeffrey, Flauger, Raphael, Foreman, Simon, Fuller, George, Garcia, Marcos AG, García-Bellido, Juan, Gerbino, Martina, Gluscevic, Vera, Gontcho, Satya Gontcho A, Górski, Krzysztof M, Grin, Daniel, Grohs, Evan, Gudmundsson, Jon E, Hanany, Shaul, Handley, Will, Hill, J Colin, Hirata, Christopher M, Hložek, Renée, Holder, Gilbert, Horiuchi, Shunsaku, Huterer, Dragan, Kadota, Kenji, Kamionkowski, Marc, Keeley, Ryan E, Khatri, Rishi, Kisner, Theodore, Kneib, Jean-Paul, Knox, Lloyd, Koushiappas, Savvas M, Kovetz, Ely D, L'Huillier, Benjamin, Lahav, Ofer, Lattanzi, Massimiliano, Lee, Hayden, Liguori, Michele, Lin, Tongyan, Loverde, Marilena, Madhavacheril, Mathew, Masui, Kiyoshi, McMahon, Jeff, McQuinn, Matthew, Meerburg, P Daniel, Mirbabayi, Mehrdad, Motloch, Pavel, Mukherjee, Suvodip, Munõz, Julian B, Nagy, Johanna, Newburgh, Laura, Niemack, Michael D, Nomerotski, Andrei, Page, Lyman, Piacentni, Francesco, Pierpaoli, Elena, Pogosian, Levon, Pryke, Clement, Green, Daniel, Green, Daniel, Amin, Mustafa A, Meyers, Joel, Wallisch, Benjamin, Abazajian, Kevork N, Abidi, Muntazir, Adshead, Peter, Ahmed, Zeeshan, Ansarinejad, Behzad, Armstrong, Robert, Baccigalupi, Carlo, Bandura, Kevin, Barron, Darcy, Battaglia, Nicholas, Baumann, Daniel, Bechtol, Keith, Bennett, Charles, Benson, Bradford, Beutler, Florian, Bischoff, Colin, Bleem, Lindsey, Bond, J Richard, Borrill, Julian, Buckley-Geer, Elizabeth, Burgess, Cliff, Carlstrom, John E, Castorina, Emanuele, Challinor, Anthony, Chen, Xingang, Cooray, Asantha, Coulton, William, Craig, Nathaniel, Crawford, Thomas, Cyr-Racine, Francis-Yan, D'Amico, Guido, Demarteau, Marcel, Doré, Olivier, Yutong, Duan, Dunkley, Joanna, Dvorkin, Cora, Ellison, John, Engelen, Alexander van, Escoffier, Stephanie, Essinger-Hileman, Tom, Fabbian, Giulio, Filippini, Jeffrey, Flauger, Raphael, Foreman, Simon, Fuller, George, Garcia, Marcos AG, García-Bellido, Juan, Gerbino, Martina, Gluscevic, Vera, Gontcho, Satya Gontcho A, Górski, Krzysztof M, Grin, Daniel, Grohs, Evan, Gudmundsson, Jon E, Hanany, Shaul, Handley, Will, Hill, J Colin, Hirata, Christopher M, Hložek, Renée, Holder, Gilbert, Horiuchi, Shunsaku, Huterer, Dragan, Kadota, Kenji, Kamionkowski, Marc, Keeley, Ryan E, Khatri, Rishi, Kisner, Theodore, Kneib, Jean-Paul, Knox, Lloyd, Koushiappas, Savvas M, Kovetz, Ely D, L'Huillier, Benjamin, Lahav, Ofer, Lattanzi, Massimiliano, Lee, Hayden, Liguori, Michele, Lin, Tongyan, Loverde, Marilena, Madhavacheril, Mathew, Masui, Kiyoshi, McMahon, Jeff, McQuinn, Matthew, Meerburg, P Daniel, Mirbabayi, Mehrdad, Motloch, Pavel, Mukherjee, Suvodip, Munõz, Julian B, Nagy, Johanna, Newburgh, Laura, Niemack, Michael D, Nomerotski, Andrei, Page, Lyman, Piacentni, Francesco, Pierpaoli, Elena, Pogosian, Levon, and Pryke, Clement
Abstract: The hot dense environment of the early universe is known to have produced large numbers of baryons, photons, and neutrinos. These extreme conditions may have also produced other long-lived species, including new light particles (such as axions or sterile neutrinos) or gravitational waves. The gravitational effects of any such light relics can be observed through their unique imprint in the cosmic microwave background (CMB), the large-scale structure, and the primordial light element abundances, and are important in determining the initial conditions of the universe. We argue that future cosmological observations, in particular improved maps of the CMB on small angular scales, can be orders of magnitude more sensitive for probing the thermal history of the early universe than current experiments. These observations offer a unique and broad discovery space for new physics in the dark sector and beyond, even when its effects would not be visible in terrestrial experiments or in astrophysical environments. A detection of an excess light relic abundance would be a clear indication of new physics and would provide the first direct information about the universe between the times of reheating and neutrino decoupling one second later.
Published: 2019

33. Black holes, gravitational waves and fundamental physics : a roadmap

Author: Barack, Leor, Cardoso, Vitor, Nissanke, Samaya, Sotiriou, Thomas P., Askar, Abbas, Belczynski, Chris, Bertone, Gianfranco, Bon, Edi, Blas, Diego, Brito, Richard, Bulik, Tomasz, Burrage, Clare, Byrnes, Christian T., Caprini, Chiara, Chernyakova, Masha, Chruściel, Piotr, Colpi, Monica, Ferrari, Valeria, Gaggero, Daniele, Gair, Jonathan, García-Bellido, Juan, Hassan, Sayed Fawad, Heisenberg, Lavinia, Hendry, Martin, Heng, Ik Siong, Herdeiro, Carlos, Hinderer, Tanja, Horesh, Assaf, Kavanagh, Bradley J., Kocsis, Bence, Kramer, Michael, Le Tiec, Alexandre, Mingarelli, Chiara, Nardini, Germano, Nelemans, Gijs, Palenzuela, Carlos, Pani, Paolo, Perego, Albino, Porter, Edward K., Rossi, Elena M., Schmidt, Patricia, Sesana, Alberto, Sperhake, Ulrich, Stamerra, Antonio, Stein, Leo C., Tamanini, Nicola, Tauris, Thomas M., Arturo Urena-López, L., Vincent, Frederic, Volonteri, Marta, Wardell, Barry, Wex, Norbert, Yagi, Kent, Abdelsalhin, Tiziano, Ángel Aloy, Miguel, Amaro-Seoane, Pau, Annulli, Lorenzo, Arca-Sedda, Manuel, Bah, Ibrahima, Barausse, Enrico, Barakovic, Elvis, Benkel, Robert, Bennett, Charles L., Bernard, Laura, Bernuzzi, Sebastiano, Berry, Christopher P. L., Berti, Emanuele, Bezares, Miguel, Juan Blanco-Pillado, Jose, Blázquez-Salcedo, Jose Luis, Bonetti, Matteo, Bošković, Mateja, Bosnjak, Zeljka, Bricman, Katja, Brügmann, Bernd, Capelo, Pedro R., Carloni, Sante, Cerdá-Durán, Pablo, Charmousis, Christos, Chaty, Sylvain, Clerici, Aurora, Coates, Andrew, Colleoni, Marta, Collodel, Lucas G., Compère, Geoffrey, Cook, William, Cordero-Carríon, Isabel, Correia, Miguel, de la Cruz-Dombriz, Álvaro, Czinner, Viktor G., Destounis, Kyriakos, Dialektopoulos, Kostas, Doneva, Daniela, Dotti, Massimo, Drew, Amelia, Eckner, Christopher, Edholm, James, Emparan, Roberto, Erdem, Recai, Ferreira, Miguel, Ferreira, Pedro G., Finch, Andrew, Font, Jose A., Franchini, Nicola, Fransen, Kwinten, Gal'tsov, Dmitry, Ganguly, Apratim, Gerosa, Davide, Glampedakis, Kostas, Gomboc, Andreja, Goobar, Ariel, Gualtieri, Leonardo, Guendelman, Eduardo, Haardt, Francesco, Harmark, Troels, Hejda, Filip, Hertog, Thomas, Hopper, Seth, Husa, Sascha, Ihanec, Nada, Ikeda, Taishi, Jaodand, Amruta, Jetzer, Philippe, Jimenez-Forteza, Xisco, Kamionkowski, Marc, Kaplan, David E., Kazantzidis, Stelios, Kimura, Masashi, Kobayashi, Shiho, Kokkotas, Kostas, Krolik, Julian, Kunz, Jutta, Lämmerzahl, Claus, Lasky, Paul, Lemos, José P. S., Said, Jackson Levi, Liberati, Stefano, Lopes, Jorge, Luna, Raimon, Ma, Yin-Zhe, Maggio, Elisa, Mangiagli, Alberto, Montero, Marina Martinez, Maselli, Andrea, Mayer, Lucio, Mazumdar, Anupam, Messenger, Christopher, Ménard, Brice, Minamitsuji, Masato, Moore, Christopher J., Mota, David, Nampalliwar, Sourabh, Nerozzi, Andrea, Nichols, David, Nissimov, Emil, Obergaulinger, Martin, Obers, Niels A., Oliveri, Roberto, Pappas, George, Pasic, Vedad, Peiris, Hiranya, Petrushevska, Tanja, Pollney, Denis, Pratten, Geraint, Rakic, Nemanja, Racz, Istvan, Radia, Miren, Ramazanoglu, Fethi M., Ramos-Buades, Antoni, Raposo, Guilherme, Rogatko, Marek, Rosca-Mead, Roxana, Rosinska, Dorota, Rosswog, Stephan, Ruiz-Morales, Ester, Sakellariadou, Mairi, Sanchis-Gual, Nicolás, Salafia, Om Sharan, Samajdar, Anuradha, Sintes, Alicia, Smole, Majda, Sopuerta, Carlos, Souza-Lima, Rafael, Stalevski, Marko, Stergioulas, Nikolaos, Stevens, Chris, Tamfal, Tomas, Torres-Forne, Alejandro, Tsygankov, Sergey, Ünlütürk, Kivanç I., Valiante, Rosa, van de Meent, Maarten, Velhinho, José, Verbin, Yosef, Vercnocke, Bert, Vernieri, Daniele, Vicente, Rodrigo, Vitagliano, Vincenzo, Weltman, Amanda, Whiting, Bernard, Williamson, Andrew, Witek, Helvi, Wojnar, Aneta, Yakut, Kadri, Yan, Haopeng, Yazadjiev, Stoycho, Zaharijas, Gabrijela, Zilhão, Miguel, Barack, Leor, Cardoso, Vitor, Nissanke, Samaya, Sotiriou, Thomas P., Askar, Abbas, Belczynski, Chris, Bertone, Gianfranco, Bon, Edi, Blas, Diego, Brito, Richard, Bulik, Tomasz, Burrage, Clare, Byrnes, Christian T., Caprini, Chiara, Chernyakova, Masha, Chruściel, Piotr, Colpi, Monica, Ferrari, Valeria, Gaggero, Daniele, Gair, Jonathan, García-Bellido, Juan, Hassan, Sayed Fawad, Heisenberg, Lavinia, Hendry, Martin, Heng, Ik Siong, Herdeiro, Carlos, Hinderer, Tanja, Horesh, Assaf, Kavanagh, Bradley J., Kocsis, Bence, Kramer, Michael, Le Tiec, Alexandre, Mingarelli, Chiara, Nardini, Germano, Nelemans, Gijs, Palenzuela, Carlos, Pani, Paolo, Perego, Albino, Porter, Edward K., Rossi, Elena M., Schmidt, Patricia, Sesana, Alberto, Sperhake, Ulrich, Stamerra, Antonio, Stein, Leo C., Tamanini, Nicola, Tauris, Thomas M., Arturo Urena-López, L., Vincent, Frederic, Volonteri, Marta, Wardell, Barry, Wex, Norbert, Yagi, Kent, Abdelsalhin, Tiziano, Ángel Aloy, Miguel, Amaro-Seoane, Pau, Annulli, Lorenzo, Arca-Sedda, Manuel, Bah, Ibrahima, Barausse, Enrico, Barakovic, Elvis, Benkel, Robert, Bennett, Charles L., Bernard, Laura, Bernuzzi, Sebastiano, Berry, Christopher P. L., Berti, Emanuele, Bezares, Miguel, Juan Blanco-Pillado, Jose, Blázquez-Salcedo, Jose Luis, Bonetti, Matteo, Bošković, Mateja, Bosnjak, Zeljka, Bricman, Katja, Brügmann, Bernd, Capelo, Pedro R., Carloni, Sante, Cerdá-Durán, Pablo, Charmousis, Christos, Chaty, Sylvain, Clerici, Aurora, Coates, Andrew, Colleoni, Marta, Collodel, Lucas G., Compère, Geoffrey, Cook, William, Cordero-Carríon, Isabel, Correia, Miguel, de la Cruz-Dombriz, Álvaro, Czinner, Viktor G., Destounis, Kyriakos, Dialektopoulos, Kostas, Doneva, Daniela, Dotti, Massimo, Drew, Amelia, Eckner, Christopher, Edholm, James, Emparan, Roberto, Erdem, Recai, Ferreira, Miguel, Ferreira, Pedro G., Finch, Andrew, Font, Jose A., Franchini, Nicola, Fransen, Kwinten, Gal'tsov, Dmitry, Ganguly, Apratim, Gerosa, Davide, Glampedakis, Kostas, Gomboc, Andreja, Goobar, Ariel, Gualtieri, Leonardo, Guendelman, Eduardo, Haardt, Francesco, Harmark, Troels, Hejda, Filip, Hertog, Thomas, Hopper, Seth, Husa, Sascha, Ihanec, Nada, Ikeda, Taishi, Jaodand, Amruta, Jetzer, Philippe, Jimenez-Forteza, Xisco, Kamionkowski, Marc, Kaplan, David E., Kazantzidis, Stelios, Kimura, Masashi, Kobayashi, Shiho, Kokkotas, Kostas, Krolik, Julian, Kunz, Jutta, Lämmerzahl, Claus, Lasky, Paul, Lemos, José P. S., Said, Jackson Levi, Liberati, Stefano, Lopes, Jorge, Luna, Raimon, Ma, Yin-Zhe, Maggio, Elisa, Mangiagli, Alberto, Montero, Marina Martinez, Maselli, Andrea, Mayer, Lucio, Mazumdar, Anupam, Messenger, Christopher, Ménard, Brice, Minamitsuji, Masato, Moore, Christopher J., Mota, David, Nampalliwar, Sourabh, Nerozzi, Andrea, Nichols, David, Nissimov, Emil, Obergaulinger, Martin, Obers, Niels A., Oliveri, Roberto, Pappas, George, Pasic, Vedad, Peiris, Hiranya, Petrushevska, Tanja, Pollney, Denis, Pratten, Geraint, Rakic, Nemanja, Racz, Istvan, Radia, Miren, Ramazanoglu, Fethi M., Ramos-Buades, Antoni, Raposo, Guilherme, Rogatko, Marek, Rosca-Mead, Roxana, Rosinska, Dorota, Rosswog, Stephan, Ruiz-Morales, Ester, Sakellariadou, Mairi, Sanchis-Gual, Nicolás, Salafia, Om Sharan, Samajdar, Anuradha, Sintes, Alicia, Smole, Majda, Sopuerta, Carlos, Souza-Lima, Rafael, Stalevski, Marko, Stergioulas, Nikolaos, Stevens, Chris, Tamfal, Tomas, Torres-Forne, Alejandro, Tsygankov, Sergey, Ünlütürk, Kivanç I., Valiante, Rosa, van de Meent, Maarten, Velhinho, José, Verbin, Yosef, Vercnocke, Bert, Vernieri, Daniele, Vicente, Rodrigo, Vitagliano, Vincenzo, Weltman, Amanda, Whiting, Bernard, Williamson, Andrew, Witek, Helvi, Wojnar, Aneta, Yakut, Kadri, Yan, Haopeng, Yazadjiev, Stoycho, Zaharijas, Gabrijela, and Zilhão, Miguel
Abstract: The grand challenges of contemporary fundamental physics dark matter, dark energy, vacuum energy, inflation and early universe cosmology, singularities and the hierarchy problem all involve gravity as a key component. And of all gravitational phenomena, black holes stand out in their elegant simplicity, while harbouring some of the most remarkable predictions of General Relativity: event horizons, singularities and ergoregions. The hitherto invisible landscape of the gravitational Universe is being unveiled before our eyes: the historical direct detection of gravitational waves by the LIGO-Virgo collaboration marks the dawn of a new era of scientific exploration. Gravitational-wave astronomy will allow us to test models of black hole formation, growth and evolution, as well as models of gravitational-wave generation and propagation. It will provide evidence for event horizons and ergoregions, test the theory of General Relativity itself, and may reveal the existence of new fundamental fields. The synthesis of these results has the potential to radically reshape our understanding of the cosmos and of the laws of Nature. The purpose of this work is to present a concise, yet comprehensive overview of the state of the art in the relevant fields of research, summarize important open problems, and lay out a roadmap for future progress. This write-up is an initiative taken within the framework of the European Action on 'Black holes, Gravitational waves and Fundamental Physics'.
Published: 2019
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34. Two-year Cosmology Large Angular Scale Surveyor (CLASS) Observations: A First Detection of Atmospheric Circular Polarization at Q Band

Author: Petroff, Matthew A., Eimer, Joseph R., Harrington, Kathleen, Ali, Aamir, Appel, John W., Bennett, Charles L., Brewer, Michael K., Bustos, Ricardo, Chan, Manwei, Chuss, David T., Cleary, Joseph, Couto, Jullianna Denes, Dahal, Sumit, Dünner, Rolando, Essinger-Hileman, Thomas, Rojas, Pedro Fluxá, Gothe, Dominik, Iuliano, Jeffrey, Marriage, Tobias A., Miller, Nathan J., Núñez, Carolina, Padilla, Ivan L., Parker, Lucas, Reeves, Rodrigo, Rostem, Karwan, Valle, Deniz Augusto Nunes, Watts, Duncan J., Weiland, Janet L., Wollack, Edward J., Xu, Zhilei, Petroff, Matthew A., Eimer, Joseph R., Harrington, Kathleen, Ali, Aamir, Appel, John W., Bennett, Charles L., Brewer, Michael K., Bustos, Ricardo, Chan, Manwei, Chuss, David T., Cleary, Joseph, Couto, Jullianna Denes, Dahal, Sumit, Dünner, Rolando, Essinger-Hileman, Thomas, Rojas, Pedro Fluxá, Gothe, Dominik, Iuliano, Jeffrey, Marriage, Tobias A., Miller, Nathan J., Núñez, Carolina, Padilla, Ivan L., Parker, Lucas, Reeves, Rodrigo, Rostem, Karwan, Valle, Deniz Augusto Nunes, Watts, Duncan J., Weiland, Janet L., Wollack, Edward J., and Xu, Zhilei
Abstract: The Earth's magnetic field induces Zeeman splitting of the magnetic dipole transitions of molecular oxygen in the atmosphere, which produces polarized emission in the millimeter-wave regime. This polarized emission is primarily circularly polarized and manifests as a foreground with a dipole-shaped sky pattern for polarization-sensitive ground-based cosmic microwave background experiments, such as the Cosmology Large Angular Scale Surveyor (CLASS), which is capable of measuring large angular scale circular polarization. Using atmospheric emission theory and radiative transfer formalisms, we model the expected amplitude and spatial distribution of this signal and evaluate the model for the CLASS observing site in the Atacama Desert of northern Chile. Then, using two years of observations at 32.3 GHz to 43.7 GHz from the CLASS Q-band telescope, we present a detection of this signal and compare the observed signal to that predicted by the model. We recover an angle between magnetic north and true north of $(-5.5 \pm 0.6)^\circ$, which is consistent with the expectation of $-5.9^\circ$ for the CLASS observing site. When comparing dipole sky patterns fit to both simulated and data-derived sky maps, the dipole directions match to within a degree, and the measured amplitudes match to within ${\sim}20\%$., Comment: 13 pages, 7 figures, published in ApJ
Published: 2019
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35. Two-year Cosmology Large Angular Scale Surveyor (CLASS) Observations: 40 GHz Telescope Pointing, Beam Profile, Window Function, and Polarization Performance

Author: Xu, Zhilei, Brewer, Michael K., Rojas, Pedro Fluxá, Li, Yunyang, Osumi, Keisuke, Pradenas, Bastián, Ali, Aamir, Appel, John W., Bennett, Charles L., Bustos, Ricardo, Chan, Manwei, Chuss, David T., Cleary, Joseph, Couto, Jullianna Denes, Dahal, Sumit, Datta, Rahul, Denis, Kevin L., Dünner, Rolando, Eimer, Joseph R., Essinger-Hileman, Thomas, Gothe, Dominik, Harrington, Kathleen, Iuliano, Jeffrey, Karakla, John, Marriage, Tobias A., Miller, Nathan J., Núñez, Carolina, Padilla, Ivan L., Parker, Lucas, Petroff, Matthew A., Reeves, Rodrigo, Rostem, Karwan, Valle, Deniz Augusto Nunes, Watts, Duncan J., Weiland, Janet, Wollack, Edward J., Xu, Zhilei, Brewer, Michael K., Rojas, Pedro Fluxá, Li, Yunyang, Osumi, Keisuke, Pradenas, Bastián, Ali, Aamir, Appel, John W., Bennett, Charles L., Bustos, Ricardo, Chan, Manwei, Chuss, David T., Cleary, Joseph, Couto, Jullianna Denes, Dahal, Sumit, Datta, Rahul, Denis, Kevin L., Dünner, Rolando, Eimer, Joseph R., Essinger-Hileman, Thomas, Gothe, Dominik, Harrington, Kathleen, Iuliano, Jeffrey, Karakla, John, Marriage, Tobias A., Miller, Nathan J., Núñez, Carolina, Padilla, Ivan L., Parker, Lucas, Petroff, Matthew A., Reeves, Rodrigo, Rostem, Karwan, Valle, Deniz Augusto Nunes, Watts, Duncan J., Weiland, Janet, and Wollack, Edward J.
Abstract: The Cosmology Large Angular Scale Surveyor (CLASS) is a telescope array that observes the cosmic microwave background (CMB) over 75% of the sky from the Atacama Desert, Chile, at frequency bands centered near 40, 90, 150, and 220 GHz. CLASS measures the large angular scale ($1^\circ\lesssim\theta\leqslant 90^\circ$) CMB polarization to constrain the tensor-to-scalar ratio at the $r\sim0.01$ level and the optical depth to last scattering to the sample variance limit. This paper presents the optical characterization of the 40 GHz telescope during its first observation era, from 2016 September to 2018 February. High signal-to-noise observations of the Moon establish the pointing and beam calibration. The telescope boresight pointing variation is $<0.023^\circ$ ($<1.6$% of the beam's full width at half maximum (FWHM)). We estimate beam parameters per detector and in aggregate, as in the CMB survey maps. The aggregate beam has an FWHM of $1.579^\circ\pm.001^\circ$ and a solid angle of $838 \pm 6\ \mu{\rm sr}$, consistent with physical optics simulations. The corresponding beam window function has a sub-percent error per multipole at $\ell < 200$. An extended $90^\circ$ beam map reveals no significant far sidelobes. The observed Moon polarization shows that the instrument polarization angles are consistent with the optical model and that the temperature-to-polarization leakage fraction is $<10^{-4}$ (95% C.L.). We find that the Moon-based results are consistent with measurements of M42, RCW 38, and Tau A from CLASS's CMB survey data. In particular, Tau A measurements establish degree-level precision for instrument polarization angles., Comment: 32 pages, 24 figures, published in ApJ
Published: 2019
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36. Two-year Cosmology Large Angular Scale Surveyor (CLASS) Observations: A Measurement of Circular Polarization at 40 GHz

Author: Padilla, Ivan L., Eimer, Joseph R., Li, Yunyang, Addison, Graeme E., Ali, Aamir, Appel, John W., Bennett, Charles L., Bustos, Ricardo, Brewer, Michael K., Chan, Manwei, Chuss, David T., Cleary, Joseph, Couto, Jullianna, Dahal, Sumit, Denis, Kevin, Dünner, Rolando, Essinger-Hileman, Thomas, Fluxá, Pedro, Haridas, Saianeesh K., Harrington, Kathleen, Iuliano, Jeffrey, Karakla, John, Marriage, Tobias A., Miller, Nathan J., Núñez, Carolina, Parker, Lucas, Petroff, Matthew A., Reeves, Rodrigo, Rostem, Karwan, Stevens, Robert W., Valle, Deniz Augusto Nunes, Watts, Duncan J., Weiland, Janet L., Wollack, Edward J., Xu, Zhilei, Padilla, Ivan L., Eimer, Joseph R., Li, Yunyang, Addison, Graeme E., Ali, Aamir, Appel, John W., Bennett, Charles L., Bustos, Ricardo, Brewer, Michael K., Chan, Manwei, Chuss, David T., Cleary, Joseph, Couto, Jullianna, Dahal, Sumit, Denis, Kevin, Dünner, Rolando, Essinger-Hileman, Thomas, Fluxá, Pedro, Haridas, Saianeesh K., Harrington, Kathleen, Iuliano, Jeffrey, Karakla, John, Marriage, Tobias A., Miller, Nathan J., Núñez, Carolina, Parker, Lucas, Petroff, Matthew A., Reeves, Rodrigo, Rostem, Karwan, Stevens, Robert W., Valle, Deniz Augusto Nunes, Watts, Duncan J., Weiland, Janet L., Wollack, Edward J., and Xu, Zhilei
Abstract: We report circular polarization measurements from the first two years of observation with the 40 GHz polarimeter of the Cosmology Large Angular Scale Surveyor (CLASS). CLASS is conducting a multi-frequency survey covering 75% of the sky from the Atacama Desert designed to measure the cosmic microwave background (CMB) linear E and B polarization on angular scales $1^\circ \lesssim \theta \leq 90^\circ$, corresponding to a multipole range of $2 \leq \ell \lesssim 200$. The modulation technology enabling measurements of linear polarization at the largest angular scales from the ground, the Variable-delay Polarization Modulator, is uniquely designed to provide explicit sensitivity to circular polarization (Stokes $V$). We present a first detection of circularly polarized atmospheric emission at 40 GHz that is well described by a dipole with an amplitude of $124\pm4\,\mathrm{\mu K}$ when observed at an elevation of $45^\circ$, and discuss its potential impact as a foreground to CMB experiments. Filtering the atmospheric component, CLASS places a 95% C.L. upper limit of $0.4\,\mathrm{\mu K}^2$ to $13.5\,\mathrm{\mu K}^2$ on $\ell(\ell+1)C_\ell^{VV}/(2\pi)$ between $1 \leq \ell \leq 120$, representing a two-orders-of-magnitude improvement over previous limits., Comment: 8 pages, 5 figures
Published: 2019
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37. Analytic Calculation of Covariance between Cosmological Parameters from Correlated Data Sets, with an Application to SPTpol

Author: Kable, Joshua A., Addison, Graeme E., Bennett, Charles L., Kable, Joshua A., Addison, Graeme E., and Bennett, Charles L.
Abstract: Consistency checks of cosmological data sets are an important tool because they may suggest systematic errors or the type of modifications to $\Lambda$CDM necessary to resolve current tensions. In this work, we derive an analytic method for calculating the level of correlations between model parameters from two correlated cosmological data sets, which complements more computationally expensive simulations. This method is an extension of the Fisher analysis that assumes a Gaussian likelihood and a known data covariance matrix. We apply this method to the SPTpol temperature and polarization CMB spectra (TE and EE). We find weak correlations between $\Lambda$CDM parameters with a 9$\%$ correlation between the TE-only and EE-only constraints on $H_0$ and a 25$\%$ and 32$\%$ correlation for log($A_s$) and $n_s$ respectively. Despite the negative correlations between the TE and EE power spectra, the correlations in the parameters are positive. The TE-EE parameter differences are consistent with zero, with a PTE of 0.53, in contrast to the PTE of 0.017 reported by SPTpol for the consistency of the TE and EE power spectra with $\Lambda$CDM. Using simulations we find that the results of these two tests are independent and that this difference can arise simply from statistical fluctuations. Ignoring correlations in the TT-TE and TE-EE comparisons biases the $\chi^2$ low, artificially making parameters look more consistent. Therefore, we conclude that these correlations need to be accounted for when performing internal consistency checks of the TT vs TE vs EE power spectra for future CMB analyses., Comment: 13 pages, 6 figures, Published by ApJ
Published: 2019
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38. The CLASS 150/220 GHz Polarimeter Array: Design, Assembly, and Characterization

Author: Dahal, Sumit, Amiri, Mandana, Appel, John W., Bennett, Charles L., Corbett, Lance, Datta, Rahul, Denis, Kevin, Essinger-Hileman, Thomas, Halpern, Mark, Helson, Kyle, Hilton, Gene, Hubmayr, Johannes, Keller, Benjamin, Marriage, Tobias, Nunez, Carolina, Petroff, Matthew, Reintsema, Carl, Rostem, Karwan, U-Yen, Kongpop, Wollack, Edward, Dahal, Sumit, Amiri, Mandana, Appel, John W., Bennett, Charles L., Corbett, Lance, Datta, Rahul, Denis, Kevin, Essinger-Hileman, Thomas, Halpern, Mark, Helson, Kyle, Hilton, Gene, Hubmayr, Johannes, Keller, Benjamin, Marriage, Tobias, Nunez, Carolina, Petroff, Matthew, Reintsema, Carl, Rostem, Karwan, U-Yen, Kongpop, and Wollack, Edward
Abstract: We report on the development of a polarization-sensitive dichroic (150/220 GHz) detector array for the Cosmology Large Angular Scale Surveyor (CLASS) delivered to the telescope site in June 2019. In concert with existing 40 and 90 GHz telescopes, the 150/220 GHz telescope will make observations of the cosmic microwave background over large angular scales aimed at measuring the primordial B-mode signal, the optical depth to reionization, and other fundamental physics and cosmology. The 150/220 GHz focal plane array consists of three detector modules with 1020 transition edge sensor (TES) bolometers in total. Each dual-polarization pixel on the focal plane contains four bolometers to measure the two linear polarization states at 150 and 220 GHz. Light is coupled through a planar orthomode transducer (OMT) fed by a smooth-walled feedhorn array made from an aluminum-silicon alloy (CE7). In this work, we discuss the design, assembly, and in-lab characterization of the 150/220 GHz detector array. The detectors are photon-noise limited, and we estimate the total array noise-equivalent power (NEP) to be 2.5 and 4 aW$\sqrt{\mathrm{s}}$ for 150 and 220 GHz arrays, respectively., Comment: 8 pages, 5 figures, Published in J Low Temp Phys
Published: 2019
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39. Accounting for Correlations When Fitting Extra Cosmological Parameters

Author: Huang, Yajing, Addison, Graeme, Bennett, Charles, Huang, Yajing, Addison, Graeme, and Bennett, Charles
Abstract: Current cosmological tensions motivate investigating extensions to the standard $\Lambda$CDM model. Additional model parameters are typically varied one or two at a time, in a series of separate tests. The purpose of this paper is to highlight that information is lost by not also examining the correlations between these additional parameters, which arise when their effects on model predictions are similar, even if the parameters are not varied simultaneously. We show how these correlations can be quantified with simulations and Markov Chain Monte Carlo (MCMC) methods. As an example, we assume that $\Lambda$CDM is the true underlying model, and calculate the correlations expected between the phenomenological lensing amplitude parameter, $A_L$, the running of the spectral index, $n_{\rm run}$, and the primordial helium mass fraction, $Y_P$, when these parameters are varied one at a time along with the $\Lambda$CDM parameters in fits to the $\textit{Planck}$ 2015 temperature power spectrum. These correlations are not small, ranging from 0.31 ($A_L-n_{\rm run}$) to $-0.93$ ($n_{\rm run}-Y_P$). We find that the values of these three parameters from the $\textit{Planck}$ data are consistent with $\Lambda$CDM expectations within $0.9\sigma$ when the correlations are accounted for. This does not explain the 1.8-2.7$\sigma$ $\textit{Planck}$ preference for $A_L>1$, but provides an additional $\Lambda$CDM consistency test. For example, if $A_L>1$ was a symptom of an underlying systematic error or some real but unknown physical effect that also produced spurious correlations with $n_{\rm run}$ or $Y_P$ our test might have revealed this. We recommend that future cosmological analyses examine correlations between additional model parameters in addition to investigating them separately, one a time.
Published: 2019
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40. Caveat medicus:Clinician experiences in publishing reports of serious oncology-associated adverse drug reactions

Author: Bennett, Charles L., Schooley, Benjamin, Taylor, Matthew A., Witherspoon, Bartlett J., Godwin, Ashley, Vemula, Jayanth, Ausdenmoore, Henry C., Sartor, Oliver, Tony Yang, Y., Armitage, James O., Hrushesky, William J., Restaino, John, Thomsen, Henrik S., Yarnold, Paul R., Young, Terence, Knopf, Kevin B., Chen, Brian, Bennett, Charles L., Schooley, Benjamin, Taylor, Matthew A., Witherspoon, Bartlett J., Godwin, Ashley, Vemula, Jayanth, Ausdenmoore, Henry C., Sartor, Oliver, Tony Yang, Y., Armitage, James O., Hrushesky, William J., Restaino, John, Thomsen, Henrik S., Yarnold, Paul R., Young, Terence, Knopf, Kevin B., and Chen, Brian
Abstract: Oncology-associated adverse drug/device reactions can be fatal. Some clinicians who treat single patients with severe oncology-associated toxicities have researched case series and published this information. We investigated motivations and experiences of select individuals leading such efforts. Clinicians treating individual patients who developed oncology-associated serious adverse drug events were asked to participate. Inclusion criteria included having index patient information, reporting case series, and being collaborative with investigators from two National Institutes of Health funded pharmacovigilance networks. Thirty-minute interviews addressed investigational motivation, feedback from pharmaceutical manufacturers, FDA personnel, and academic leadership, and recommendations for improving pharmacovigilance. Responses were analyzed using constant comparative methods of qualitative analysis. Overall, 18 clinicians met inclusion criteria and 14 interviewees are included. Primary motivations were scientific curiosity, expressed by six clinicians. A less common theme was public health related (three clinicians). Six clinicians received feedback characterized as supportive from academic leaders, while four clinicians received feedback characterized as negative. Three clinicians reported that following the case series publication they were invited to speak at academic institutions worldwide. Responses from pharmaceutical manufacturers were characterized as negative by 12 clinicians. One clinician’s wife called the post-reporting time the “Maalox month,” while another clinician reported that the manufacturer collaboratively offered to identify additional cases of the toxicity. Responses from FDA employees were characterized as collaborative for two clinicians, neutral for five clinicians, unresponsive for negative by six clinicians. Three clinicians endorsed developing improved reporting mechanisms for individual physicians, while 11 clinicians endorsed safety a
Published: 2019

41. Black holes, gravitational waves and fundamental physics: A roadmap

Author: Barack, L, Cardoso, V, Nissanke, S, Sotiriou, T, Askar, A, Belczynski, C, Bertone, G, Bon, E, Blas, D, Brito, R, Bulik, T, Burrage, C, Byrnes, C, Caprini, C, Chernyakova, M, Chruściel, P, Colpi, M, Ferrari, V, Gaggero, D, Gair, J, García-Bellido, J, Hassan, S, Heisenberg, L, Hendry, M, Heng, I, Herdeiro, C, Hinderer, T, Horesh, A, Kavanagh, B, Kocsis, B, Kramer, M, Le Tiec, A, Mingarelli, C, Nardini, G, Nelemans, G, Palenzuela, C, Pani, P, Perego, A, Porter, E, Rossi, E, Schmidt, P, Sesana, A, Sperhake, U, Stamerra, A, Stein, L, Tamanini, N, Tauris, T, Urena-López, L, Vincent, F, Volonteri, M, Wardell, B, Wex, N, Yagi, K, Abdelsalhin, T, Aloy, M, Amaro-Seoane, P, Annulli, L, Arca-Sedda, M, Bah, I, Barausse, E, Barakovic, E, Benkel, R, Bennett, C, Bernard, L, Bernuzzi, S, Berry, C, Berti, E, Bezares, M, Blanco-Pillado, J, Blázquez-Salcedo, J, Bonetti, M, Bošković, M, Bosnjak, Z, Bricman, K, Brügmann, B, Capelo, P, Carloni, S, Cerdá-Durán, P, Charmousis, C, Chaty, S, Clerici, A, Coates, A, Colleoni, M, Collodel, L, Compère, G, Cook, W, Cordero-Carrión, I, Correia, M, de la Cruz-Dombriz, Á, Czinner, V, Destounis, K, Dialektopoulos, K, Doneva, D, Dotti, M, Drew, A, Eckner, C, Edholm, J, Emparan, R, Erdem, R, Ferreira, M, Ferreira, P, Finch, A, Font, J, Franchini, N, Fransen, K, Gal’Tsov, D, Ganguly, A, Gerosa, D, Glampedakis, K, Gomboc, A, Goobar, A, Gualtieri, L, Guendelman, E, Haardt, F, Harmark, T, Hejda, F, Hertog, T, Hopper, S, Husa, S, Ihanec, N, Ikeda, T, Jaodand, A, Jetzer, P, Jimenez-Forteza, X, Kamionkowski, M, Kaplan, D, Kazantzidis, S, Kimura, M, Kobayashi, S, Kokkotas, K, Krolik, J, Kunz, J, Lämmerzahl, C, Lasky, P, Lemos, J, Levi Said, J, Liberati, S, Lopes, J, Luna, R, Ma, Y, Maggio, E, Mangiagli, A, Montero, M, Maselli, A, Mayer, L, Mazumdar, A, Messenger, C, Ménard, B, Minamitsuji, M, Moore, C, Mota, D, Nampalliwar, S, Nerozzi, A, Nichols, D, Nissimov, E, Obergaulinger, M, Obers, N, Oliveri, R, Pappas, G, Pasic, V, Peiris, H, Petrushevska, T, Pollney, D, Pratten, G, Rakic, N, Racz, I, Radia, M, Ramazanoğlu, F, Ramos-Buades, A, Raposo, G, Rogatko, M, Rosca-Mead, R, Rosinska, D, Rosswog, S, Ruiz-Morales, E, Sakellariadou, M, Sanchis-Gual, N, Sharan Salafia, O, Samajdar, A, Sintes, A, Smole, M, Sopuerta, C, Souza-Lima, R, Stalevski, M, Stergioulas, N, Stevens, C, Tamfal, T, Torres-Forné, A, Tsygankov, S, İ Ünlütürk, K, Valiante, R, van de Meent, M, Velhinho, J, Verbin, Y, Vercnocke, B, Vernieri, D, Vicente, R, Vitagliano, V, Weltman, A, Whiting, B, Williamson, A, Witek, H, Wojnar, A, Yakut, K, Yan, H, Yazadjiev, S, Zaharijas, G, Zilhão, M, Barack, Leor, Cardoso, Vitor, Nissanke, Samaya, Sotiriou, Thomas P, Askar, Abbas, Belczynski, Chris, Bertone, Gianfranco, Bon, Edi, Blas, Diego, Brito, Richard, Bulik, Tomasz, Burrage, Clare, Byrnes, Christian T, Caprini, Chiara, Chernyakova, Masha, Chruściel, Piotr, Colpi, Monica, Ferrari, Valeria, Gaggero, Daniele, Gair, Jonathan, García-Bellido, Juan, Hassan, S F, Heisenberg, Lavinia, Hendry, Martin, Heng, Ik Siong, Herdeiro, Carlos, Hinderer, Tanja, Horesh, Assaf, Kavanagh, Bradley J, Kocsis, Bence, Kramer, Michael, Le Tiec, Alexandre, Mingarelli, Chiara, Nardini, Germano, Nelemans, Gijs, Palenzuela, Carlos, Pani, Paolo, Perego, Albino, Porter, Edward K, Rossi, Elena M, Schmidt, Patricia, Sesana, Alberto, Sperhake, Ulrich, Stamerra, Antonio, Stein, Leo C, Tamanini, Nicola, Tauris, Thomas M, Urena-López, L Arturo, Vincent, Frederic, Volonteri, Marta, Wardell, Barry, Wex, Norbert, Yagi, Kent, Abdelsalhin, Tiziano, Aloy, Miguel Ángel, Amaro-Seoane, Pau, Annulli, Lorenzo, Arca-Sedda, Manuel, Bah, Ibrahima, Barausse, Enrico, Barakovic, Elvis, Benkel, Robert, Bennett, Charles L, Bernard, Laura, Bernuzzi, Sebastiano, Berry, Christopher P L, Berti, Emanuele, Bezares, Miguel, Blanco-Pillado, Jose Juan, Blázquez-Salcedo, Jose Luis, Bonetti, Matteo, Bošković, Mateja, Bosnjak, Zeljka, Bricman, Katja, Brügmann, Bernd, Capelo, Pedro R, Carloni, Sante, Cerdá-Durán, Pablo, Charmousis, Christos, Chaty, Sylvain, Clerici, Aurora, Coates, Andrew, Colleoni, Marta, Collodel, Lucas G, Compère, Geoffrey, Cook, William, Cordero-Carrión, Isabel, Correia, Miguel, de la Cruz-Dombriz, Álvaro, Czinner, Viktor G, Destounis, Kyriakos, Dialektopoulos, Kostas, Doneva, Daniela, Dotti, Massimo, Drew, Amelia, Eckner, Christopher, Edholm, James, Emparan, Roberto, Erdem, Recai, Ferreira, Miguel, Ferreira, Pedro G, Finch, Andrew, Font, Jose A, Franchini, Nicola, Fransen, Kwinten, Gal’tsov, Dmitry, Ganguly, Apratim, Gerosa, Davide, Glampedakis, Kostas, Gomboc, Andreja, Goobar, Ariel, Gualtieri, Leonardo, Guendelman, Eduardo, Haardt, Francesco, Harmark, Troels, Hejda, Filip, Hertog, Thomas, Hopper, Seth, Husa, Sascha, Ihanec, Nada, Ikeda, Taishi, Jaodand, Amruta, Jetzer, Philippe, Jimenez-Forteza, Xisco, Kamionkowski, Marc, Kaplan, David E, Kazantzidis, Stelios, Kimura, Masashi, Kobayashi, Shiho, Kokkotas, Kostas, Krolik, Julian, Kunz, Jutta, Lämmerzahl, Claus, Lasky, Paul, Lemos, José P S, Levi Said, Jackson, Liberati, Stefano, Lopes, Jorge, Luna, Raimon, Ma, Yin-Zhe, Maggio, Elisa, Mangiagli, Alberto, Montero, Marina Martinez, Maselli, Andrea, Mayer, Lucio, Mazumdar, Anupam, Messenger, Christopher, Ménard, Brice, Minamitsuji, Masato, Moore, Christopher J, Mota, David, Nampalliwar, Sourabh, Nerozzi, Andrea, Nichols, David, Nissimov, Emil, Obergaulinger, Martin, Obers, Niels A, Oliveri, Roberto, Pappas, George, Pasic, Vedad, Peiris, Hiranya, Petrushevska, Tanja, Pollney, Denis, Pratten, Geraint, Rakic, Nemanja, Racz, Istvan, Radia, Miren, Ramazanoğlu, Fethi M, Ramos-Buades, Antoni, Raposo, Guilherme, Rogatko, Marek, Rosca-Mead, Roxana, Rosinska, Dorota, Rosswog, Stephan, Ruiz-Morales, Ester, Sakellariadou, Mairi, Sanchis-Gual, Nicolás, Sharan Salafia, Om, Samajdar, Anuradha, Sintes, Alicia, Smole, Majda, Sopuerta, Carlos, Souza-Lima, Rafael, Stalevski, Marko, Stergioulas, Nikolaos, Stevens, Chris, Tamfal, Tomas, Torres-Forné, Alejandro, Tsygankov, Sergey, İ Ünlütürk, Kıvanç, Valiante, Rosa, van de Meent, Maarten, Velhinho, José, Verbin, Yosef, Vercnocke, Bert, Vernieri, Daniele, Vicente, Rodrigo, Vitagliano, Vincenzo, Weltman, Amanda, Whiting, Bernard, Williamson, Andrew, Witek, Helvi, Wojnar, Aneta, Yakut, Kadri, Yan, Haopeng, Yazadjiev, Stoycho, Zaharijas, Gabrijela, Zilhão, Miguel, Barack, L, Cardoso, V, Nissanke, S, Sotiriou, T, Askar, A, Belczynski, C, Bertone, G, Bon, E, Blas, D, Brito, R, Bulik, T, Burrage, C, Byrnes, C, Caprini, C, Chernyakova, M, Chruściel, P, Colpi, M, Ferrari, V, Gaggero, D, Gair, J, García-Bellido, J, Hassan, S, Heisenberg, L, Hendry, M, Heng, I, Herdeiro, C, Hinderer, T, Horesh, A, Kavanagh, B, Kocsis, B, Kramer, M, Le Tiec, A, Mingarelli, C, Nardini, G, Nelemans, G, Palenzuela, C, Pani, P, Perego, A, Porter, E, Rossi, E, Schmidt, P, Sesana, A, Sperhake, U, Stamerra, A, Stein, L, Tamanini, N, Tauris, T, Urena-López, L, Vincent, F, Volonteri, M, Wardell, B, Wex, N, Yagi, K, Abdelsalhin, T, Aloy, M, Amaro-Seoane, P, Annulli, L, Arca-Sedda, M, Bah, I, Barausse, E, Barakovic, E, Benkel, R, Bennett, C, Bernard, L, Bernuzzi, S, Berry, C, Berti, E, Bezares, M, Blanco-Pillado, J, Blázquez-Salcedo, J, Bonetti, M, Bošković, M, Bosnjak, Z, Bricman, K, Brügmann, B, Capelo, P, Carloni, S, Cerdá-Durán, P, Charmousis, C, Chaty, S, Clerici, A, Coates, A, Colleoni, M, Collodel, L, Compère, G, Cook, W, Cordero-Carrión, I, Correia, M, de la Cruz-Dombriz, Á, Czinner, V, Destounis, K, Dialektopoulos, K, Doneva, D, Dotti, M, Drew, A, Eckner, C, Edholm, J, Emparan, R, Erdem, R, Ferreira, M, Ferreira, P, Finch, A, Font, J, Franchini, N, Fransen, K, Gal’Tsov, D, Ganguly, A, Gerosa, D, Glampedakis, K, Gomboc, A, Goobar, A, Gualtieri, L, Guendelman, E, Haardt, F, Harmark, T, Hejda, F, Hertog, T, Hopper, S, Husa, S, Ihanec, N, Ikeda, T, Jaodand, A, Jetzer, P, Jimenez-Forteza, X, Kamionkowski, M, Kaplan, D, Kazantzidis, S, Kimura, M, Kobayashi, S, Kokkotas, K, Krolik, J, Kunz, J, Lämmerzahl, C, Lasky, P, Lemos, J, Levi Said, J, Liberati, S, Lopes, J, Luna, R, Ma, Y, Maggio, E, Mangiagli, A, Montero, M, Maselli, A, Mayer, L, Mazumdar, A, Messenger, C, Ménard, B, Minamitsuji, M, Moore, C, Mota, D, Nampalliwar, S, Nerozzi, A, Nichols, D, Nissimov, E, Obergaulinger, M, Obers, N, Oliveri, R, Pappas, G, Pasic, V, Peiris, H, Petrushevska, T, Pollney, D, Pratten, G, Rakic, N, Racz, I, Radia, M, Ramazanoğlu, F, Ramos-Buades, A, Raposo, G, Rogatko, M, Rosca-Mead, R, Rosinska, D, Rosswog, S, Ruiz-Morales, E, Sakellariadou, M, Sanchis-Gual, N, Sharan Salafia, O, Samajdar, A, Sintes, A, Smole, M, Sopuerta, C, Souza-Lima, R, Stalevski, M, Stergioulas, N, Stevens, C, Tamfal, T, Torres-Forné, A, Tsygankov, S, İ Ünlütürk, K, Valiante, R, van de Meent, M, Velhinho, J, Verbin, Y, Vercnocke, B, Vernieri, D, Vicente, R, Vitagliano, V, Weltman, A, Whiting, B, Williamson, A, Witek, H, Wojnar, A, Yakut, K, Yan, H, Yazadjiev, S, Zaharijas, G, Zilhão, M, Barack, Leor, Cardoso, Vitor, Nissanke, Samaya, Sotiriou, Thomas P, Askar, Abbas, Belczynski, Chris, Bertone, Gianfranco, Bon, Edi, Blas, Diego, Brito, Richard, Bulik, Tomasz, Burrage, Clare, Byrnes, Christian T, Caprini, Chiara, Chernyakova, Masha, Chruściel, Piotr, Colpi, Monica, Ferrari, Valeria, Gaggero, Daniele, Gair, Jonathan, García-Bellido, Juan, Hassan, S F, Heisenberg, Lavinia, Hendry, Martin, Heng, Ik Siong, Herdeiro, Carlos, Hinderer, Tanja, Horesh, Assaf, Kavanagh, Bradley J, Kocsis, Bence, Kramer, Michael, Le Tiec, Alexandre, Mingarelli, Chiara, Nardini, Germano, Nelemans, Gijs, Palenzuela, Carlos, Pani, Paolo, Perego, Albino, Porter, Edward K, Rossi, Elena M, Schmidt, Patricia, Sesana, Alberto, Sperhake, Ulrich, Stamerra, Antonio, Stein, Leo C, Tamanini, Nicola, Tauris, Thomas M, Urena-López, L Arturo, Vincent, Frederic, Volonteri, Marta, Wardell, Barry, Wex, Norbert, Yagi, Kent, Abdelsalhin, Tiziano, Aloy, Miguel Ángel, Amaro-Seoane, Pau, Annulli, Lorenzo, Arca-Sedda, Manuel, Bah, Ibrahima, Barausse, Enrico, Barakovic, Elvis, Benkel, Robert, Bennett, Charles L, Bernard, Laura, Bernuzzi, Sebastiano, Berry, Christopher P L, Berti, Emanuele, Bezares, Miguel, Blanco-Pillado, Jose Juan, Blázquez-Salcedo, Jose Luis, Bonetti, Matteo, Bošković, Mateja, Bosnjak, Zeljka, Bricman, Katja, Brügmann, Bernd, Capelo, Pedro R, Carloni, Sante, Cerdá-Durán, Pablo, Charmousis, Christos, Chaty, Sylvain, Clerici, Aurora, Coates, Andrew, Colleoni, Marta, Collodel, Lucas G, Compère, Geoffrey, Cook, William, Cordero-Carrión, Isabel, Correia, Miguel, de la Cruz-Dombriz, Álvaro, Czinner, Viktor G, Destounis, Kyriakos, Dialektopoulos, Kostas, Doneva, Daniela, Dotti, Massimo, Drew, Amelia, Eckner, Christopher, Edholm, James, Emparan, Roberto, Erdem, Recai, Ferreira, Miguel, Ferreira, Pedro G, Finch, Andrew, Font, Jose A, Franchini, Nicola, Fransen, Kwinten, Gal’tsov, Dmitry, Ganguly, Apratim, Gerosa, Davide, Glampedakis, Kostas, Gomboc, Andreja, Goobar, Ariel, Gualtieri, Leonardo, Guendelman, Eduardo, Haardt, Francesco, Harmark, Troels, Hejda, Filip, Hertog, Thomas, Hopper, Seth, Husa, Sascha, Ihanec, Nada, Ikeda, Taishi, Jaodand, Amruta, Jetzer, Philippe, Jimenez-Forteza, Xisco, Kamionkowski, Marc, Kaplan, David E, Kazantzidis, Stelios, Kimura, Masashi, Kobayashi, Shiho, Kokkotas, Kostas, Krolik, Julian, Kunz, Jutta, Lämmerzahl, Claus, Lasky, Paul, Lemos, José P S, Levi Said, Jackson, Liberati, Stefano, Lopes, Jorge, Luna, Raimon, Ma, Yin-Zhe, Maggio, Elisa, Mangiagli, Alberto, Montero, Marina Martinez, Maselli, Andrea, Mayer, Lucio, Mazumdar, Anupam, Messenger, Christopher, Ménard, Brice, Minamitsuji, Masato, Moore, Christopher J, Mota, David, Nampalliwar, Sourabh, Nerozzi, Andrea, Nichols, David, Nissimov, Emil, Obergaulinger, Martin, Obers, Niels A, Oliveri, Roberto, Pappas, George, Pasic, Vedad, Peiris, Hiranya, Petrushevska, Tanja, Pollney, Denis, Pratten, Geraint, Rakic, Nemanja, Racz, Istvan, Radia, Miren, Ramazanoğlu, Fethi M, Ramos-Buades, Antoni, Raposo, Guilherme, Rogatko, Marek, Rosca-Mead, Roxana, Rosinska, Dorota, Rosswog, Stephan, Ruiz-Morales, Ester, Sakellariadou, Mairi, Sanchis-Gual, Nicolás, Sharan Salafia, Om, Samajdar, Anuradha, Sintes, Alicia, Smole, Majda, Sopuerta, Carlos, Souza-Lima, Rafael, Stalevski, Marko, Stergioulas, Nikolaos, Stevens, Chris, Tamfal, Tomas, Torres-Forné, Alejandro, Tsygankov, Sergey, İ Ünlütürk, Kıvanç, Valiante, Rosa, van de Meent, Maarten, Velhinho, José, Verbin, Yosef, Vercnocke, Bert, Vernieri, Daniele, Vicente, Rodrigo, Vitagliano, Vincenzo, Weltman, Amanda, Whiting, Bernard, Williamson, Andrew, Witek, Helvi, Wojnar, Aneta, Yakut, Kadri, Yan, Haopeng, Yazadjiev, Stoycho, Zaharijas, Gabrijela, and Zilhão, Miguel
Abstract: The grand challenges of contemporary fundamental physics-dark matter, dark energy, vacuum energy, inflation and early universe cosmology, singularities and the hierarchy problem-all involve gravity as a key component. And of all gravitational phenomena, black holes stand out in their elegant simplicity, while harbouring some of the most remarkable predictions of General Relativity: event horizons, singularities and ergoregions. The hitherto invisible landscape of the gravitational Universe is being unveiled before our eyes: the historical direct detection of gravitational waves by the LIGO-Virgo collaboration marks the dawn of a new era of scientific exploration. Gravitational-wave astronomy will allow us to test models of black hole formation, growth and evolution, as well as models of gravitational-wave generation and propagation. It will provide evidence for event horizons and ergoregions, test the theory of General Relativity itself, and may reveal the existence of new fundamental fields. The synthesis of these results has the potential to radically reshape our understanding of the cosmos and of the laws of Nature. The purpose of this work is to present a concise, yet comprehensive overview of the state of the art in the relevant fields of research, summarize important open problems, and lay out a roadmap for future progress. This write-up is an initiative taken within the framework of the European Action on 'Black holes, Gravitational waves and Fundamental Physics'.
Published: 2019

42. Black holes, gravitational waves and fundamental physics: a roadmap

Author: Ramazanoğlu, Fethi Mübin (ORCID 0000-0003-3075-1457 & YÖK ID 254225); Ünlütürk, Kıvanç İbrahim, Barack, Leor; Cardoso, Vitor; Nissanke, Samaya; Sotiriou, Thomas P.; Askar, Abbas; Belczynski, Chris; Bertone, Gianfranco; Bon, Edi; Blas, Diego; Brito, Richard; Bulik, Tomasz; Burrage, Clare; Byrnes, Christian T.; Caprini, Chiara; Chernyakova, Masha; Chrusciel, Piotr; Colpi, Monica; Ferrari, Valeria; Gaggero, Daniele; Gair, Jonathan; Garcia-Bellido, Juan; Hassan, S. F.; Heisenberg, Lavinia; Hendry, Martin; Heng, Ik Siong; Herdeiro, Carlos; Hinderer, Tanja; Horesh, Assaf; Kavanagh, Bradley J.; Kocsis, Bence; Kramer, Michael; Le Tiec, Alexandre; Mingarelli, Chiara; Nardini, Germano; Nelemans, Gijs; Palenzuela, Carlos; Pani, Paolo; Perego, Albino; Porter, Edward K.; Rossi, Elena M.; Schmidt, Patricia; Sesana, Alberto; Sperhake, Ulrich; Stamerra, Antonio; Stein, Leo C.; Tamanini, Nicola; Tauris, Thomas M.; Arturo Urena-Lopez, L.; Vincent, Frederic; Volonteri, Marta; Wardell, Barry; Wex, Norbert; Yagi, Kent; Abdelsalhin, Tiziano; Angel Aloy, Miguel; Amaro-Seoane, Pau; Annulli, Lorenzo; Arca-Sedda, Manuel; Bah, Ibrahima; Barausse, Enrico; Barakovic, Elvis; Benkel, Robert; Bennett, Charles L.; Bernard, Laura; Bernuzzi, Sebastiano; Berry, Christopher P. L.; Berti, Emanuele; Bezares, Miguel; Juan Blanco-Pillado, Jose; Blazquez-Salcedo, Jose Luis; Bonetti, Matteo; Boskovic, Mateja; Bosnjak, Zeljka; Bricman, Katja; Bruegmann, Bernd; Capelo, Pedro R.; Carloni, Sante; Cerda-Duran, Pablo; Charmousis, Christos; Chaty, Sylvain; Clerici, Aurora; Coates, Andrew; Colleoni, Marta; Collodel, Lucas G.; Compere, Geoffrey; Cook, William; Cordero-Carrion, Isabel; Correia, Miguel; de la Cruz-Dombriz, Alvaro; Czinner, Viktor G.; Destounis, Kyriakos; Dialektopoulos, Kostas; Doneva, Daniela; Dotti, Massimo; Drew, Amelia; Eckner, Christopher; Edholm, James; Emparan, Roberto; Erdem, Recai; Ferreira, Miguel; Ferreira, Pedro G.; Finch, Andrew; Font, Jose A.; Franchini, Nicola; Fransen, Kwinten; Gal'tsov, Dmitry; Ganguly, Apratim; Gerosa, Davide; Glampedakis, Kostas; Gomboc, Andreja; Goobar, Ariel, College of Sciences; Graduate School of Sciences and Engineering, Department of Physics, Ramazanoğlu, Fethi Mübin (ORCID 0000-0003-3075-1457 & YÖK ID 254225); Ünlütürk, Kıvanç İbrahim, Barack, Leor; Cardoso, Vitor; Nissanke, Samaya; Sotiriou, Thomas P.; Askar, Abbas; Belczynski, Chris; Bertone, Gianfranco; Bon, Edi; Blas, Diego; Brito, Richard; Bulik, Tomasz; Burrage, Clare; Byrnes, Christian T.; Caprini, Chiara; Chernyakova, Masha; Chrusciel, Piotr; Colpi, Monica; Ferrari, Valeria; Gaggero, Daniele; Gair, Jonathan; Garcia-Bellido, Juan; Hassan, S. F.; Heisenberg, Lavinia; Hendry, Martin; Heng, Ik Siong; Herdeiro, Carlos; Hinderer, Tanja; Horesh, Assaf; Kavanagh, Bradley J.; Kocsis, Bence; Kramer, Michael; Le Tiec, Alexandre; Mingarelli, Chiara; Nardini, Germano; Nelemans, Gijs; Palenzuela, Carlos; Pani, Paolo; Perego, Albino; Porter, Edward K.; Rossi, Elena M.; Schmidt, Patricia; Sesana, Alberto; Sperhake, Ulrich; Stamerra, Antonio; Stein, Leo C.; Tamanini, Nicola; Tauris, Thomas M.; Arturo Urena-Lopez, L.; Vincent, Frederic; Volonteri, Marta; Wardell, Barry; Wex, Norbert; Yagi, Kent; Abdelsalhin, Tiziano; Angel Aloy, Miguel; Amaro-Seoane, Pau; Annulli, Lorenzo; Arca-Sedda, Manuel; Bah, Ibrahima; Barausse, Enrico; Barakovic, Elvis; Benkel, Robert; Bennett, Charles L.; Bernard, Laura; Bernuzzi, Sebastiano; Berry, Christopher P. L.; Berti, Emanuele; Bezares, Miguel; Juan Blanco-Pillado, Jose; Blazquez-Salcedo, Jose Luis; Bonetti, Matteo; Boskovic, Mateja; Bosnjak, Zeljka; Bricman, Katja; Bruegmann, Bernd; Capelo, Pedro R.; Carloni, Sante; Cerda-Duran, Pablo; Charmousis, Christos; Chaty, Sylvain; Clerici, Aurora; Coates, Andrew; Colleoni, Marta; Collodel, Lucas G.; Compere, Geoffrey; Cook, William; Cordero-Carrion, Isabel; Correia, Miguel; de la Cruz-Dombriz, Alvaro; Czinner, Viktor G.; Destounis, Kyriakos; Dialektopoulos, Kostas; Doneva, Daniela; Dotti, Massimo; Drew, Amelia; Eckner, Christopher; Edholm, James; Emparan, Roberto; Erdem, Recai; Ferreira, Miguel; Ferreira, Pedro G.; Finch, Andrew; Font, Jose A.; Franchini, Nicola; Fransen, Kwinten; Gal'tsov, Dmitry; Ganguly, Apratim; Gerosa, Davide; Glampedakis, Kostas; Gomboc, Andreja; Goobar, Ariel, College of Sciences; Graduate School of Sciences and Engineering, and Department of Physics
Abstract: The grand challenges of contemporary fundamental physics dark matter, dark energy, vacuum energy, inflation and early universe cosmology, singularities and the hierarchy problem all involve gravity as a key component. And of all gravitational phenomena, black holes stand out in their elegant simplicity, while harbouring some of the most remarkable predictions of General Relativity: event horizons, singularities and ergoregions.The hitherto invisible landscape of the gravitational Universe is being unveiled before our eyes: the historical direct detection of gravitational waves by the LIGO-Virgo collaboration marks the dawn of a new era of scientific exploration. Gravitational-wave astronomy will allow us to test models of black hole formation, growth and evolution, as well as models of gravitational-wave generation and propagation. It will provide evidence for event horizons and ergoregions, test the theory of General Relativity itself, and may reveal the existence of new fundamental fields. The synthesis of these results has the potential to radically reshape our understanding of the cosmos and of the laws of Nature.The purpose of this work is to present a concise, yet comprehensive overview of the state of the art in the relevant fields of research, summarize important open problems, and lay out a roadmap for future progress., European Union (EU); European Cooperation in Science and Technology (COST); Polish National Science Center (NCN); Carl Tryggers Foundation; Science & Technology Facilities Council (STFC); European Union's H2020 ERC Consolidator Grant 'Matter and strong-field gravity: New frontiers in Einstein's theory'; European Research Council (ERC); Horizon 2020; Science & Technology Facilities Council (STFC; Ministry of Education and Science of the Republic of Serbia; Foundation for Polish Science; Austrian Science Fund (FWF); Polish National Center of Science (NCN); European Research Council (ERC); Hungarian National Research, Development, and Innovation Office; Swiss National Science Foundation (SNSF); European Union's H2020 ERC; H2020-MSCA-RISE-2015 Grant; National Science Foundation (NSF); PRACE; Simons Foundation; Ministry of Economy, Industry and Competitiveness of Spain; Slovenian Research Agency - Slovenia; EU H2020 under ERC; Spanish MINECO; Generalitat Valenciana; NASA by the Chandra X-ray Center; National Aeronautics & Space Administration (NASA); Scientific and Technological Research Council of Turkey (TÜBİTAK); H2020-MSCA-RISE-2017 Grant; Scientific and Technological Research Council of Turkey (TÜBİTAK); National Science Centre of Poland - European Union; Deutscher Akademischer Austausch Dienst (DAAD); GWAVES of ARIS-GRNET(Athens); Royal Society of London; Research Grant; Scientific and Technological Research Council of Turkey (TÜBİTAK)
Published: 2019

43. Quantum Cryptography II: How to re-use a one-time pad safely even if P=NP

Author: Bennett, Charles, Brassard, Gilles, Breidbart, Seth, Bennett, Charles, Brassard, Gilles, and Breidbart, Seth
Abstract: When elementary quantum systems, such as polarized photons, are used to transmit digital information, the uncertainty principle gives rise to novel cryptographic phenomena unachievable with traditional transmission media, e.g.acommunications channel on which it is impossible in principle to eavesdrop without a high probability of being detected. With such a channel, a one-time pad can safely be reused many times as long as no eavesdrop is detected, and, planning ahead, part of the capacity of these uncompromised transmissions can be used to send fresh random bits with which to replace the one-time pad when an eavesdrop finally is detected. Unlike other schemes for stretching a one-time pad, this scheme does not depend on complexity-theoretic assumptions such as the difficulty of factoring.
Published: 2019

44. Process Guide for Student Involvement in Historical Research.

Author: Scituate School Dist., North Scituate, RI., Bennett, Charles, and Lenihan, J. Michael
Abstract: The booklet describes the local history component of an interdisciplinary high school course on American Studies. The program involves students over a three-year period in collecting, recording, organizing, interpreting, and disseminating the history, culture, and tradition of Scituate, Rhode Island. The booklet is presented in six chapters. Chapter I stresses that local and state history should be taught in high school and discusses how this project can be adapted to the needs of other school systems. Chapter II emphasizes the need for teaching about historiography and outlines a unit on historical method. Chapter III suggests sources of information for local history projects, including local libraries, social organizations, newspaper files, town clerk's offices, family records, state or local historical societies, recorded interviews, and local historical sites. Chapter IV suggests student activities such as field trips, interviewing local citizens, workshops, and disseminating information about the project in the community. Chapter V recommends equipment and materials such as cameras, film, slide projectors, and cassette tapes. The final chapter offers suggestions for evaluating local history projects. Evaluation procedures should include pre- and posttests on historiography and local history, standardized tests on U.S. history and American literature, and questionnaires dealing with student interest in the project. (Author/DB)
Published: 1977

45. Black holes, gravitational waves and fundamental physics: a roadmap

Author: Barack, Leor, Cardoso, Vitor, Nissanke, Samaya, Sotiriou, Thomas P., Askar, Abbas, Belczynski, Krzysztof, Bertone, Gianfranco, Bon, Edi, Blas, Diego, Brito, Richard, Bulik, Tomasz, Burrage, Clare, Byrnes, Christian T., Caprini, Chiara, Chernyakova, Masha, Chrusciel, Piotr, Colpi, Monica, Ferrari, Valeria, Gaggero, Daniele, Gair, Jonathan, Garcia-Bellido, Juan, Hassan, S. F., Heisenberg, Lavinia, Hendry, Martin, Heng, Ik Siong, Herdeiro, Carlos, Hinderer, Tanja, Horesh, Assaf, Kavanagh, Bradley J., Kocsis, Bence, Kramer, Michael, Tiec, Alexandre Le, Mingarelli, Chiara, Nardini, Germano, Nelemans, Gijs, Palenzuela, Carlos, Pani, Paolo, Perego, Albino, Porter, Edward K., Rossi, Elena M., Schmidt, Patricia, Sesana, Alberto, Sperhake, Ulrich, Stamerra, Antonio, Stein, Leo C., Tamanini, Nicola, Tauris, Thomas M., Urena-Lopez, L. Arturo, Vincent, Frederic, Volonteri, Marta, Wardell, Barry, Wex, Norbert, Yagi, Kent, Abdelsalhin, Tiziano, Aloy, Miguel Angel, Amaro-Seoane, Pau, Annulli, Lorenzo, Arca-Sedda, Manuel, Bah, Ibrahima, Barausse, Enrico, Barakovic, Elvis, Benkel, Robert, Bennett, Charles L., Bernard, Laura, Bernuzzi, Sebastiano, Berry, Christopher P. L., Berti, Emanuele, Bezares, Miguel, Blanco-Pillado, Jose Juan, Blazquez-Salcedo, Jose Luis, Bonetti, Matteo, Boskovic, Mateja, Bosnjak, Zeljka, Bricman, Katja, Bruegmann, Bernd, Capelo, Pedro R., Carloni, Sante, Cerda-Duran, Pablo, Charmousis, Christos, Chaty, Sylvain, Clerici, Aurora, Coates, Andrew, Colleoni, Marta, Collodel, Lucas G., Compere, Geoffrey, Cook, William, Cordero-Carrion, Isabel, Correia, Miguel, de la Cruz-Dombriz, Alvaro, Czinner, Viktor G., Destounis, Kyriakos, Dialektopoulos, Kostas, Doneva, Daniela, Dotti, Massimo, Drew, Amelia, Eckner, Christopher, Edholm, James, Emparan, Roberto, Erdem, Recai, Ferreira, Miguel, Ferreira, Pedro G., Finch, Andrew, Font, Jose A., Franchini, Nicola, Fransen, Kwinten, Gal'tsov, Dmitry, Ganguly, Apratim, Gerosa, Davide, Glampedakis, Kostas, Gomboc, Andreja, Goobar, Ariel, Gualtieri, Leonardo, Guendelman, Eduardo, Haardt, Francesco, Harmark, Troels, Hejda, Filip, Hertog, Thomas, Hopper, Seth, Husa, Sascha, Ihanec, Nada, Ikeda, Taishi, Jaodand, Amruta, Jimenez-Forteza, Philippe Jetzer Xisco, Kamionkowski, Marc, Kaplan, David E., Kazantzidis, Stelios, Kimura, Masashi, Kobayashi, Shiho, Kokkotas, Kostas, Krolik, Julian, Kunz, Jutta, Lammerzahl, Claus, Lasky, Paul, Lemos, Jose P. S., Said, Jackson Levi, Liberati, Stefano, Lopes, Jorge, Luna, Raimon, Ma, Yin-Zhe, Maggio, Elisa, Montero, Marina Martinez, Maselli, Andrea, Mayer, Lucio, Mazumdar, Anupam, Messenger, Christopher, Menard, Brice, Minamitsuji, Masato, Moore, Christopher J., Mota, David, Nampalliwar, Sourabh, Nerozzi, Andrea, Nichols, David, Nissimov, Emil, Obergaulinger, Martin, Obers, Niels A., Oliveri, Roberto, Pappas, George, Pasic, Vedad, Peiris, Hiranya, Petrushevska, Tanja, Pollney, Denis, Pratten, Geraint, Rakic, Nemanja, Racz, Istvan, Radia, Miren, Ramazanouglu, Fethi M., Ramos-Buades, Antoni, Raposo, Guilherme, Rosca-Mead, Roxana, Rogatko, Marek, Rosinska, Dorota, Rosswog, Stephan, Morales, Ester Ruiz, Sakellariadou, Mairi, Sanchis-Gual, Nicolas, Salafia, Om Sharan, Samajdar, Anuradha, Sintes, Alicia, Smole, Majda, Sopuerta, Carlos, Souza-Lima, Rafael, Stalevski, Marko, Stergioulas, Nikolaos, Stevens, Chris, Tamfal, Tomas, Torres-Forne, Alejandro, Tsygankov, Sergey, Unluturk, Kivanc, Valiante, Rosa, van de Meent, Maarten, Velhinho, Jose, Verbin, Yosef, Vercnocke, Bert, Vernieri, Daniele, Vicente, Rodrigo, Vitagliano, Vincenzo, Weltman, Amanda, Whiting, Bernard, Williamson, Andrew, Witek, Helvi, Wojnar, Aneta, Yakut, Kadri, Yan, Haopeng, Yazadjiev, Stoycho, Zaharijas, Gabrijela, Zilhao, Miguel, Barack, Leor, Cardoso, Vitor, Nissanke, Samaya, Sotiriou, Thomas P., Askar, Abbas, Belczynski, Krzysztof, Bertone, Gianfranco, Bon, Edi, Blas, Diego, Brito, Richard, Bulik, Tomasz, Burrage, Clare, Byrnes, Christian T., Caprini, Chiara, Chernyakova, Masha, Chrusciel, Piotr, Colpi, Monica, Ferrari, Valeria, Gaggero, Daniele, Gair, Jonathan, Garcia-Bellido, Juan, Hassan, S. F., Heisenberg, Lavinia, Hendry, Martin, Heng, Ik Siong, Herdeiro, Carlos, Hinderer, Tanja, Horesh, Assaf, Kavanagh, Bradley J., Kocsis, Bence, Kramer, Michael, Tiec, Alexandre Le, Mingarelli, Chiara, Nardini, Germano, Nelemans, Gijs, Palenzuela, Carlos, Pani, Paolo, Perego, Albino, Porter, Edward K., Rossi, Elena M., Schmidt, Patricia, Sesana, Alberto, Sperhake, Ulrich, Stamerra, Antonio, Stein, Leo C., Tamanini, Nicola, Tauris, Thomas M., Urena-Lopez, L. Arturo, Vincent, Frederic, Volonteri, Marta, Wardell, Barry, Wex, Norbert, Yagi, Kent, Abdelsalhin, Tiziano, Aloy, Miguel Angel, Amaro-Seoane, Pau, Annulli, Lorenzo, Arca-Sedda, Manuel, Bah, Ibrahima, Barausse, Enrico, Barakovic, Elvis, Benkel, Robert, Bennett, Charles L., Bernard, Laura, Bernuzzi, Sebastiano, Berry, Christopher P. L., Berti, Emanuele, Bezares, Miguel, Blanco-Pillado, Jose Juan, Blazquez-Salcedo, Jose Luis, Bonetti, Matteo, Boskovic, Mateja, Bosnjak, Zeljka, Bricman, Katja, Bruegmann, Bernd, Capelo, Pedro R., Carloni, Sante, Cerda-Duran, Pablo, Charmousis, Christos, Chaty, Sylvain, Clerici, Aurora, Coates, Andrew, Colleoni, Marta, Collodel, Lucas G., Compere, Geoffrey, Cook, William, Cordero-Carrion, Isabel, Correia, Miguel, de la Cruz-Dombriz, Alvaro, Czinner, Viktor G., Destounis, Kyriakos, Dialektopoulos, Kostas, Doneva, Daniela, Dotti, Massimo, Drew, Amelia, Eckner, Christopher, Edholm, James, Emparan, Roberto, Erdem, Recai, Ferreira, Miguel, Ferreira, Pedro G., Finch, Andrew, Font, Jose A., Franchini, Nicola, Fransen, Kwinten, Gal'tsov, Dmitry, Ganguly, Apratim, Gerosa, Davide, Glampedakis, Kostas, Gomboc, Andreja, Goobar, Ariel, Gualtieri, Leonardo, Guendelman, Eduardo, Haardt, Francesco, Harmark, Troels, Hejda, Filip, Hertog, Thomas, Hopper, Seth, Husa, Sascha, Ihanec, Nada, Ikeda, Taishi, Jaodand, Amruta, Jimenez-Forteza, Philippe Jetzer Xisco, Kamionkowski, Marc, Kaplan, David E., Kazantzidis, Stelios, Kimura, Masashi, Kobayashi, Shiho, Kokkotas, Kostas, Krolik, Julian, Kunz, Jutta, Lammerzahl, Claus, Lasky, Paul, Lemos, Jose P. S., Said, Jackson Levi, Liberati, Stefano, Lopes, Jorge, Luna, Raimon, Ma, Yin-Zhe, Maggio, Elisa, Montero, Marina Martinez, Maselli, Andrea, Mayer, Lucio, Mazumdar, Anupam, Messenger, Christopher, Menard, Brice, Minamitsuji, Masato, Moore, Christopher J., Mota, David, Nampalliwar, Sourabh, Nerozzi, Andrea, Nichols, David, Nissimov, Emil, Obergaulinger, Martin, Obers, Niels A., Oliveri, Roberto, Pappas, George, Pasic, Vedad, Peiris, Hiranya, Petrushevska, Tanja, Pollney, Denis, Pratten, Geraint, Rakic, Nemanja, Racz, Istvan, Radia, Miren, Ramazanouglu, Fethi M., Ramos-Buades, Antoni, Raposo, Guilherme, Rosca-Mead, Roxana, Rogatko, Marek, Rosinska, Dorota, Rosswog, Stephan, Morales, Ester Ruiz, Sakellariadou, Mairi, Sanchis-Gual, Nicolas, Salafia, Om Sharan, Samajdar, Anuradha, Sintes, Alicia, Smole, Majda, Sopuerta, Carlos, Souza-Lima, Rafael, Stalevski, Marko, Stergioulas, Nikolaos, Stevens, Chris, Tamfal, Tomas, Torres-Forne, Alejandro, Tsygankov, Sergey, Unluturk, Kivanc, Valiante, Rosa, van de Meent, Maarten, Velhinho, Jose, Verbin, Yosef, Vercnocke, Bert, Vernieri, Daniele, Vicente, Rodrigo, Vitagliano, Vincenzo, Weltman, Amanda, Whiting, Bernard, Williamson, Andrew, Witek, Helvi, Wojnar, Aneta, Yakut, Kadri, Yan, Haopeng, Yazadjiev, Stoycho, Zaharijas, Gabrijela, and Zilhao, Miguel
Abstract: The grand challenges of contemporary fundamental physics---dark matter, dark energy, vacuum energy, inflation and early universe cosmology, singularities and the hierarchy problem---all involve gravity as a key component. And of all gravitational phenomena, black holes stand out in their elegant simplicity, while harbouring some of the most remarkable predictions of General Relativity: event horizons, singularities and ergoregions. The hitherto invisible landscape of the gravitational Universe is being unveiled before our eyes: the historical direct detection of gravitational waves by the LIGO-Virgo collaboration marks the dawn of a new era of scientific exploration. Gravitational-wave astronomy will allow us to test models of black hole formation, growth and evolution, as well as models of gravitational-wave generation and propagation. It will provide evidence for event horizons and ergoregions, test the theory of General Relativity itself, and may reveal the existence of new fundamental fields. The synthesis of these results has the potential to radically reshape our understanding of the cosmos and of the laws of Nature. The purpose of this work is to present a concise, yet comprehensive overview of the state of the art in the relevant fields of research, summarize important open problems, and lay out a roadmap for future progress., Comment: White Paper for the COST action "Gravitational Waves, Black Holes, and Fundamental Physics", 272 pages, 12 figures; v4: updated references and author list. Overall improvements and corrections. To appear in Classical and Quantum Gravity
Published: 2018
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46. On-sky performance of the CLASS Q-band telescope

Author: Appel, John W., Xu, Zhilei, Padilla, Ivan L., Harrington, Kathleen, Marquez, Bastián Pradenas, Ali, Aamir, Bennett, Charles L., Brewer, Michael K., Bustos, Ricardo, Chan, Manwei, Chuss, David T., Cleary, Joseph, Couto, Jullianna, Dahal, Sumit, Denis, Kevin, Dünner, Rolando, Eimer, Joseph R., Essinger-Hileman, Thomas, Fluxa, Pedro, Gothe, Dominik, Hilton, Gene C., Hubmayr, Johannes, Iuliano, Jeffrey, Karakla, John, Marriage, Tobias A., Miller, Nathan J., Núñez, Carolina, Parker, Lucas, Petroff, Matthew, Reintsema, Carl D., Rostem, Karwan, Stevens, Robert W., Valle, Deniz Augusto Nunes, Wang, Bingjie, Watts, Duncan J., Wollack, Edward J., Zeng, Lingzhen, Appel, John W., Xu, Zhilei, Padilla, Ivan L., Harrington, Kathleen, Marquez, Bastián Pradenas, Ali, Aamir, Bennett, Charles L., Brewer, Michael K., Bustos, Ricardo, Chan, Manwei, Chuss, David T., Cleary, Joseph, Couto, Jullianna, Dahal, Sumit, Denis, Kevin, Dünner, Rolando, Eimer, Joseph R., Essinger-Hileman, Thomas, Fluxa, Pedro, Gothe, Dominik, Hilton, Gene C., Hubmayr, Johannes, Iuliano, Jeffrey, Karakla, John, Marriage, Tobias A., Miller, Nathan J., Núñez, Carolina, Parker, Lucas, Petroff, Matthew, Reintsema, Carl D., Rostem, Karwan, Stevens, Robert W., Valle, Deniz Augusto Nunes, Wang, Bingjie, Watts, Duncan J., Wollack, Edward J., and Zeng, Lingzhen
Abstract: The Cosmology Large Angular Scale Surveyor (CLASS) is mapping the polarization of the Cosmic Microwave Background (CMB) at large angular scales ($2<\ell\lesssim200$) in search of a primordial gravitational wave B-mode signal down to a tensor-to-scalar ratio of $r \approx 0.01$. The same data set will provide a near sample-variance-limited measurement of the optical depth to reionization. Between June 2016 and March 2018, CLASS completed the largest ground-based Q-band CMB survey to date, covering over 31 000~square-degrees (75% of the sky), with an instantaneous array noise-equivalent temperature (NET) sensitivity of $32~\mu \mbox{K}_{cmb}\sqrt{\mbox{s}}$. We demonstrate that the detector optical loading ($1.6~\mbox{pW}$) and noise-equivalent power ($19~\mbox{aW}\sqrt{\mbox{s}}$) match the expected noise model dominated by photon bunching noise. We derive a $13.1\pm0.3~\mbox{K/pW}$ calibration to antenna temperature based on Moon observations, which translates to an optical efficiency of $0.48\pm0.04$ and a $27~\mbox{K}$ system noise temperature. Finally, we report a Tau A flux density of $308\pm11~\mbox{Jy}$ at $38.4\pm0.2~\mbox{GHz}$, consistent with the WMAP Tau A time-dependent spectral flux density model., Comment: 11 pages, 5 figures
Published: 2018
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47. Quantifying the CMB Degeneracy Between the Matter Density and Hubble Constant in Current Experiments

Author: Kable, Joshua A., Addison, Graeme E., Bennett, Charles L., Kable, Joshua A., Addison, Graeme E., and Bennett, Charles L.
Abstract: We revisit the degeneracy between the Hubble constant, $H_0$, and matter density, $\Omega_m$, for current cosmic microwave background (CMB) observations within the standard $\Lambda CDM$ model. We show that Planck, Wilkinson Microwave Anisotropy Probe (WMAP), South Pole Telescope (SPT), and Atacama Cosmology Telescope Polarimeter (ACTPol) temperature power spectra produce different values of the exponent $x$ from minimizing the variance of the product $\Omega_mH_0^x$. The distribution of $x$ from the different data sets does not follow the Markov Chain Monte Carlo (MCMC) best-fit values for $H_0$ or $\Omega_m$. Particularly striking is the difference between Planck multipoles $\ell\leq800$ ($x=2.81$), and WMAP ($x = 2.94$), despite very similar best-fit cosmologies. We use a Fisher matrix analysis to show that, in fact, this range in exponent values is exactly as expected in $\Lambda CDM$ given the multipole coverage and power spectrum uncertainties for each experiment. We show that the difference in $x$ from the Planck $\ell \leq 800$ and WMAP data is explained by a turning point in the relationship between $x$ and the maximum effective multipole, at around $\ell=700$. The value of $x$ is determined by several physical effects, and we highlight the significant impact of gravitational lensing for the high-multipole measurements. Despite the spread of $H_0$ values from different CMB experiments, the experiments are consistent with their sampling of the $\Omega_m-H_0$ degeneracy and do not show evidence for the need for new physics or for the presence of significant underestimated systematics according to these tests. The Fisher calculations can be used to predict the $\Omega_m-H_0$ degeneracy of future experiments., Comment: 9 pages, 6 figures, Published by ApJ
Published: 2018
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48. Design and characterization of the Cosmology Large Angular Scale Surveyor (CLASS) 93 GHz focal plane

Author: Dahal, Sumit, Ali, Aamir, Appel, John W., Essinger-Hileman, Thomas, Bennett, Charles, Brewer, Michael, Bustos, Ricardo, Chan, Manwei, Chuss, David T., Cleary, Joseph, Colazo, Felipe, Couto, Jullianna, Denis, Kevin, Dünner, Rolando, Eimer, Joseph, Engelhoven, Trevor, Fluxa, Pedro, Halpern, Mark, Harrington, Kathleen, Helson, Kyle, Hilton, Gene, Hinshaw, Gary, Hubmayr, Johannes, Iuliano, Jeffrey, Marriage, Tobias, McMahon, Jeffrey, Miller, Nathan, Nuñez, Carolina, Padilla, Ivan, Palma, Gonzalo, Parker, Lucas, Petroff, Matthew, Pradenas, Bastian, Reeves, Rodrigo, Reintsema, Carl, Rostem, Karwan, Sagliocca, Marco, U-Yen, Kongpop, Valle, Deniz, Wang, Bingjie, Wang, Qinan, Watts, Duncan, Weiland, Janet, Wollack, Edward, Xu, Zhilei, Yan, Ziang, Zen, Lingzhen, Dahal, Sumit, Ali, Aamir, Appel, John W., Essinger-Hileman, Thomas, Bennett, Charles, Brewer, Michael, Bustos, Ricardo, Chan, Manwei, Chuss, David T., Cleary, Joseph, Colazo, Felipe, Couto, Jullianna, Denis, Kevin, Dünner, Rolando, Eimer, Joseph, Engelhoven, Trevor, Fluxa, Pedro, Halpern, Mark, Harrington, Kathleen, Helson, Kyle, Hilton, Gene, Hinshaw, Gary, Hubmayr, Johannes, Iuliano, Jeffrey, Marriage, Tobias, McMahon, Jeffrey, Miller, Nathan, Nuñez, Carolina, Padilla, Ivan, Palma, Gonzalo, Parker, Lucas, Petroff, Matthew, Pradenas, Bastian, Reeves, Rodrigo, Reintsema, Carl, Rostem, Karwan, Sagliocca, Marco, U-Yen, Kongpop, Valle, Deniz, Wang, Bingjie, Wang, Qinan, Watts, Duncan, Weiland, Janet, Wollack, Edward, Xu, Zhilei, Yan, Ziang, and Zen, Lingzhen
Abstract: The Cosmology Large Angular Scale Surveyor (CLASS) aims to detect and characterize the primordial B-mode signal and make a sample-variance-limited measurement of the optical depth to reionization. CLASS is a ground-based, multi-frequency microwave polarimeter that surveys 70% of the microwave sky every day from the Atacama Desert. The focal plane detector arrays of all CLASS telescopes contain smooth-walled feedhorns that couple to transition-edge sensor (TES) bolometers through symmetric planar orthomode transducer (OMT) antennas. These low noise polarization-sensitive detector arrays are fabricated on mono-crystalline silicon wafers to maintain TES uniformity and optimize optical efficiency throughout the wafer. In this paper, we discuss the design and characterization of the first CLASS 93 GHz detector array. We measure the dark parameters, bandpass, and noise spectra of the detectors and report that the detectors are photon-noise limited. With current array yield of 82%, we estimate the total array noise-equivalent power (NEP) to be 2.1 aW$\sqrt[]{\mathrm{s}}$., Comment: 16 pages, 9 figures
Published: 2018
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49. Aerogel scattering filters for cosmic microwave background observations

Author: Essinger-Hileman, Thomas, Bennett, Charles L., Corbett, Lance, Guo, Haiquan, Helson, Kyle, Marriage, Tobias, Meador, Mary Ann B., Rostem, Karwan, Wollack, Edward J., Essinger-Hileman, Thomas, Bennett, Charles L., Corbett, Lance, Guo, Haiquan, Helson, Kyle, Marriage, Tobias, Meador, Mary Ann B., Rostem, Karwan, and Wollack, Edward J.
Abstract: We present the design and performance of broadband and tunable infrared-blocking filters for millimeter and sub-millimeter astronomy composed of small scattering particles embedded in an aerogel substrate. The ultra-low-density (typically < 150 mg/cm^3) aerogel substrate provides an index of refraction as low as 1.05, removing the need for anti-reflection coatings and allowing for broadband operation from DC to above 1 THz. The size distribution of the scattering particles can be tuned to provide a variable cutoff frequency. Aerogel filters with embedded high-resistivity silicon powder are being produced at 40-cm diameter to enable large-aperture cryogenic receivers for cosmic microwave background polarimeters, which require large arrays of sub-Kelvin detectors in their search for the signature of an inflationary gravitational-wave background., Comment: 13 pages, 5 figures, Accepted by Applied Optics
Published: 2018

50. The Cosmology Large Angular Scale Surveyor Receiver Design

Author: Iuliano, Jeffrey, Eimer, Joseph, Parker, Lucas, Rhoades, Gary, Ali, Aamir, Appel, John W., Bennett, Charles, Brewer, Michael, Bustos, Ricardo, Chuss, David, Cleary, Joseph, Couto, Jullianna, Dahal, Sumit, Denis, Kevin, Dünner, Rolando, Essinger-Hileman, Thomas, Fluxa, Pedro, Halpern, Mark, Harrington, Kathleen, Helson, Kyle, Hilton, Gene, Hinshaw, Gary, Hubmayr, Johannes, Karakla, John, Marriage, Tobias, Miller, Nathan, McMahon, Jeffrey John, Nuñez, Carolina, Padilla, Ivan, Palma, Gonzalo, Petroff, Matthew, Márquez, Bastian Pradenas, Reeves, Rodrigo, Reintsema, Carl, Rostem, Karwan, Valle, Deniz Augusto Nunes, Van Engelhoven, Trevor, Wang, Bingjie, Wang, Qinan, Watts, Duncan, Weiland, Jenet, Wollack, Edward J., Xu, Zhilei, Yan, Ziang, Zeng, Lingzhen, Iuliano, Jeffrey, Eimer, Joseph, Parker, Lucas, Rhoades, Gary, Ali, Aamir, Appel, John W., Bennett, Charles, Brewer, Michael, Bustos, Ricardo, Chuss, David, Cleary, Joseph, Couto, Jullianna, Dahal, Sumit, Denis, Kevin, Dünner, Rolando, Essinger-Hileman, Thomas, Fluxa, Pedro, Halpern, Mark, Harrington, Kathleen, Helson, Kyle, Hilton, Gene, Hinshaw, Gary, Hubmayr, Johannes, Karakla, John, Marriage, Tobias, Miller, Nathan, McMahon, Jeffrey John, Nuñez, Carolina, Padilla, Ivan, Palma, Gonzalo, Petroff, Matthew, Márquez, Bastian Pradenas, Reeves, Rodrigo, Reintsema, Carl, Rostem, Karwan, Valle, Deniz Augusto Nunes, Van Engelhoven, Trevor, Wang, Bingjie, Wang, Qinan, Watts, Duncan, Weiland, Jenet, Wollack, Edward J., Xu, Zhilei, Yan, Ziang, and Zeng, Lingzhen
Abstract: The Cosmology Large Angular Scale Surveyor consists of four instruments performing a CMB polarization survey. Currently, the 40 GHz and first 90 GHz instruments are deployed and observing, with the second 90 GHz and a multichroic 150/220 GHz instrument to follow. The receiver is a central component of each instrument's design and functionality. This paper describes the CLASS receiver design, using the first 90 GHz receiver as a primary reference. Cryogenic cooling and filters maintain a cold, low-noise environment for the detectors. We have achieved receiver detector temperatures below 50 mK in the 40 GHz instrument for 85% of the initial 1.5 years of operation, and observed in-band efficiency that is consistent with pre-deployment estimates. At 90 GHz, less than 26% of in-band power is lost to the filters and lenses in the receiver, allowing for high optical efficiency. We discuss the mounting scheme for the filters and lenses, the alignment of the cold optics and detectors, stray light control, and magnetic shielding., Comment: Fixed formatting of abstract; 20 Pages, 11 Figures, SPIE Conference Proceedings
Published: 2018
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