@article{qu_sherwin_madhavacheril_han_crowley_abril-cabezas_ade_aiola_alford_amiri_et al._2024, title={The Atacama Cosmology Telescope: A Measurement of the DR6 CMB Lensing Power Spectrum and Its Implications for Structure Growth}, volume={962}, ISSN={["1538-4357"]}, DOI={10.3847/1538-4357/acfe06}, abstractNote={Abstract}, number={2}, journal={ASTROPHYSICAL JOURNAL}, author={Qu, Frank and Sherwin, Blake D. and Madhavacheril, Mathew S. and Han, Dongwon and Crowley, Kevin T. and Abril-Cabezas, Irene and Ade, Peter A. R. and Aiola, Simone and Alford, Tommy and Amiri, Mandana and et al.}, year={2024}, month={Feb} }
@article{madhavacheril_qu_sherwin_maccrann_li_abril-cabezas_ade_aiola_alford_amiri_et al._2024, title={The Atacama Cosmology Telescope: DR6 Gravitational Lensing Map and Cosmological Parameters}, volume={962}, ISSN={["1538-4357"]}, DOI={10.3847/1538-4357/acff5f}, abstractNote={Abstract}, number={2}, journal={ASTROPHYSICAL JOURNAL}, author={Madhavacheril, Mathew S. and Qu, Frank J. and Sherwin, Blake D. and Maccrann, Niall and Li, Yaqiong and Abril-Cabezas, Irene and Ade, Peter A. R. and Aiola, Simone and Alford, Tommy and Amiri, Mandana and et al.}, year={2024}, month={Feb} }
@article{kahn_vertesi_adriaenssens_fixdal_godfrey_lumbroso_wagoner_2022, title={The Impact of Online STEM Teaching and Learning During COVID-19 on Underrepresented College Students’ Self-Efficacy and Motivation}, volume={51}, number={6}, journal={Journal of College Science Teaching}, author={Kahn, S. and Vertesi, J. and Adriaenssens, S. and Fixdal, M. and Godfrey, K. and Lumbroso, J. and Wagoner, K.}, year={2022}, month={Jul}, pages={6–15} }
@article{vavagiakis_ahmed_ali_arnold_austermann_bruno_choi_connors_cothard_dicker_et al._2021, title={The Simons Observatory: Magnetic Sensitivity Measurements of Microwave SQUID Multiplexers}, volume={31}, ISSN={1051-8223 1558-2515 2378-7074}, url={http://dx.doi.org/10.1109/TASC.2021.3069294}, DOI={10.1109/TASC.2021.3069294}, abstractNote={The Simons Observatory (SO) will be a cosmic microwave background (CMB) survey experiment with three small-aperture telescopes and one large-aperture telescope, which will observe from the Atacama Desert in Chile. In total, SO will field $\sim$70,000 transition-edge sensor (TES) bolometers in six spectral bands centered between 27 and 280 GHz in order to achieve the sensitivity necessary to measure or constrain numerous cosmological quantities. The SO Universal Focal Plane Modules (UFMs) each contain a 150 mm diameter TES detector array, horn or lenslet optical coupling, cold readout components, and magnetic shielding. SO will use a microwave SQUID multiplexing ($\mu$MUX) readout at an initial multiplexing factor of $\sim$1000; the cold (100 mK) readout components are packaged in a $\mu$MUX readout module, which is part of the UFM, and can also be characterized independently. The 100 mK stage TES bolometer arrays and microwave SQUIDs are sensitive to magnetic fields, and their measured response will vary with the degree to which they are magnetically shielded. We present measurements of the magnetic pickup of test microwave SQUID multiplexers as a study of various shielding configurations for the Simons Observatory. We discuss how these measurements motivated the material choice and design of the UFM magnetic shielding.}, number={5}, journal={IEEE Transactions on Applied Superconductivity}, publisher={Institute of Electrical and Electronics Engineers (IEEE)}, author={Vavagiakis, Eve M. and Ahmed, Zeeshan and Ali, Aamir and Arnold, Kam and Austermann, Jason and Bruno, Sarah Marie and Choi, Steve K. and Connors, Jake and Cothard, Nicholas and Dicker, Simon and et al.}, year={2021}, month={Aug}, pages={1–5} }
@book{wagoner_soden_2020, title={A New Lab for Measuring the Speed of Light}, url={http://arxiv.org/abs/2006.00330}, DOI={10.48550/arXiv.2006.00330}, abstractNote={A typical introductory treatment of electromagnetism culminates with the investigation of Maxwell's equations, showing the beautiful connection between the concepts covered in the many prior weeks. The lab described here is an experimental counterpart, providing a way to measure the connection between electricity, magnetism, and the speed of light. This is done using equipment that students have (likely) already explored in the lab and class.}, number={arXiv:2006.00330arXiv:2006.00330}, author={Wagoner, K. and Soden, R.}, year={2020} }
@book{shivam_wagoner_2020, title={How Well Do Remote Labs Work? A Case Study at Princeton University}, url={https://arxiv.org/abs/2008.04499}, DOI={10.48550/arXiv.2008.04499}, abstractNote={The onset of the COVID-19 pandemic forced many universities to move to virtual instruction during the spring 2020 semester. The transition to remote learning was abrupt and overwhelming for teachers of all subjects, all across the US. Nowhere was this more true than in science lab courses. The experience nevertheless provides an opportunity to investigate the optimal design of remote labs, with similar learning goals as in-person labs. In this study we explore the three most common approaches to remote labs: recorded experiments, applet-based experiments, and at-home projects. We use surveys and interviews to make two comparisons: remote labs vs. in-person labs; the different types of remote labs. Examining these two questions we find that remote labs perform as well as in-person labs and students learn the most from at home physics experiments while also enjoying those the most.}, number={arXiv:2008.04499arXiv:2008.04499}, author={Shivam, S. and Wagoner, K.}, year={2020} }
@article{aiola_calabrese_maurin_naess_schmitt_abitbol_addison_ade_alonso_amiri_et al._2020, title={The Atacama Cosmology Telescope: DR4 maps and cosmological parameters}, volume={2020}, ISSN={1475-7516}, url={http://dx.doi.org/10.1088/1475-7516/2020/12/047}, DOI={10.1088/1475-7516/2020/12/047}, abstractNote={We present new arcminute-resolution maps of the Cosmic Microwave Background temperature and polarization anisotropy from the Atacama Cosmology Telescope, using data taken from 2013–2016 at 98 and 150 GHz. The maps cover more than 17,000 deg2, the deepest 600 deg2 with noise levels below 10μK-arcmin. We use the power spectrum derived from almost 6,000 deg2 of these maps to constrain cosmology. The ACT data enable a measurement of the angular scale of features in both the divergence-like polarization and the temperature anisotropy, tracing both the velocity and density at last-scattering. From these one can derive the distance to the last-scattering surface and thus infer the local expansion rate, H
0. By combining ACT data with large-scale information from WMAP we measure H
0=67.6± 1.1 km/s/Mpc, at 68% confidence, in excellent agreement with the independently-measured Planck satellite estimate (from ACT alone we find H
0=67.9± 1.5 km/s/Mpc). The ΛCDM model provides a good fit to the ACT data, and we find no evidence for deviations: both the spatial curvature, and the departure from the standard lensing signal in the spectrum, are zero to within 1σ; the number of relativistic species, the primordial Helium fraction, and the running of the spectral index are consistent with ΛCDM predictions to within 1.5–2.2σ. We compare ACT, WMAP, and Planck at the parameter level and find good consistency; we investigate how the constraints on the correlated spectral index and baryon density parameters readjust when adding CMB large-scale information that ACT does not measure. The DR4 products presented here will be publicly released on the NASA Legacy Archive for Microwave Background Data Analysis.}, number={12}, journal={Journal of Cosmology and Astroparticle Physics}, publisher={IOP Publishing}, author={Aiola, Simone and Calabrese, Erminia and Maurin, Loïc and Naess, Sigurd and Schmitt, Benjamin L. and Abitbol, Maximilian H. and Addison, Graeme E. and Ade, Peter A. R. and Alonso, David and Amiri, Mandana and et al.}, year={2020}, month={Dec}, pages={047–047} }
@article{choi_hasselfield_ho_koopman_lungu_abitbol_addison_ade_aiola_alonso_et al._2020, title={The Atacama Cosmology Telescope: a measurement of the Cosmic Microwave Background power spectra at 98 and 150 GHz}, volume={2020}, ISSN={1475-7516}, url={http://dx.doi.org/10.1088/1475-7516/2020/12/045}, DOI={10.1088/1475-7516/2020/12/045}, abstractNote={We present the temperature and polarization angular power spectra of the CMB measured by the Atacama Cosmology Telescope (ACT) from 5400 deg2 of the 2013–2016 survey, which covers >15000 deg2 at 98 and 150 GHz. For this analysis we adopt a blinding strategy to help avoid confirmation bias and, related to this, show numerous checks for systematic error done before unblinding. Using the likelihood for the cosmological analysis we constrain secondary sources of anisotropy and foreground emission, and derive a “CMB-only” spectrum that extends to ℓ=4000. At large angular scales, foreground emission at 150 GHz is ∼1% of TT and EE within our selected regions and consistent with that found by Planck. Using the same likelihood, we obtain the cosmological parameters for ΛCDM for the ACT data alone with a prior on the optical depth of τ=0.065±0.015. ΛCDM is a good fit. The best-fit model has a reduced χ2 of 1.07 (PTE=0.07) with H
0=67.9±1.5 km/s/Mpc. We show that the lensing BB signal is consistent with ΛCDM and limit the celestial EB polarization angle to ψ
P
=−0.07̂±0.09̂. We directly cross correlate ACT with Planck and observe generally good agreement but with some discrepancies in TE. All data on which this analysis is based will be publicly released.}, number={12}, journal={Journal of Cosmology and Astroparticle Physics}, publisher={IOP Publishing}, author={Choi, Steve K. and Hasselfield, Matthew and Ho, Shuay-Pwu Patty and Koopman, Brian and Lungu, Marius and Abitbol, Maximilian H. and Addison, Graeme E. and Ade, Peter A. R. and Aiola, Simone and Alonso, David and et al.}, year={2020}, month={Dec}, pages={045–045} }
@inproceedings{wagoner_cowsik_huth_jeyakumar_madziwa-nussinov_abercrombie_archibald_krishnan_2019, title={Gεε Lab's Equivalence Principle Experiment}, url={http://dx.doi.org/10.22323/1.353.0043}, DOI={10.22323/1.353.0043}, abstractNote={Baron Roland von Eötvös performed amazing experiments on the equivalence of inertial and gravitational mass.Since his work experiments have become progressively more refined.The G εε Lab at Washington University in St. Louis has built a new experiment in the hopes of refining these tests even further.We have operated a prototype of this experiment by continuously monitoring the angular orientation of a torsion balance for over 115 days and the results we have obtained are promising.The experience we have gained from this experiment suggest the need for improved thermal and magnetic shielding; it also gives us confidence that long-period torsion balances have the ability to significantly improve the bounds on violation of the Equivalence Principle.Here we describe our instrument and how these experiences will be used to improve our next generation torsion balance.}, booktitle={Proceedings of International Conference on Precision Physics and Fundamental Physical Constants — PoS(FFK2019)}, publisher={Sissa Medialab}, author={Wagoner, Kasey R. and Cowsik, Ramanath and Huth, Dawson and Jeyakumar, Maneesh and Madziwa-Nussinov, Tsitsi and Abercrombie, Michael and Archibald, Adam and Krishnan, Nadathur}, year={2019}, month={Nov} }
@article{wagoner_flanagan_2019, title={Speaking of E&M}, volume={57}, ISSN={0031-921X}, url={http://dx.doi.org/10.1119/1.5088464}, DOI={10.1119/1.5088464}, abstractNote={This paper describes a new lab experiment where students explore the magnetic force on a permanent magnet placed inside a short solenoid. This lab is the fourth experiment performed in the second semester of the calculus-based introductory physics course at Washington University in St. Louis. The experiment is performed using a speaker (which students themselves have constructed), function generator, multimeter, and Vernier microphone while all analysis is done using Logger Pro. Experiments confirm a functional relationship similar to one that students have seen in class, while showing students the applicability of classroom physics to their world.}, number={2}, journal={The Physics Teacher}, publisher={American Association of Physics Teachers (AAPT)}, author={Wagoner, Kasey and Flanagan, Daniel}, year={2019}, month={Feb}, pages={78–79} }
@article{ade_aguirre_ahmed_aiola_ali_alonso_alvarez_arnold_ashton_austermann_et al._2019, title={The Simons Observatory: science goals and forecasts}, volume={2019}, ISSN={1475-7516}, url={http://dx.doi.org/10.1088/1475-7516/2019/02/056}, DOI={10.1088/1475-7516/2019/02/056}, abstractNote={The Simons Observatory (SO) is a new cosmic microwave background experiment being built on Cerro Toco in Chile, due to begin observations in the early 2020s. We describe the scientific goals of the experiment, motivate the design, and forecast its performance. SO will measure the temperature and polarization anisotropy of the cosmic microwave background in six frequency bands centered at: 27, 39, 93, 145, 225 and 280 GHz. The initial configuration of SO will have three small-aperture 0.5-m telescopes and one large-aperture 6-m telescope, with a total of 60,000 cryogenic bolometers. Our key science goals are to characterize the primordial perturbations, measure the number of relativistic species and the mass of neutrinos, test for deviations from a cosmological constant, improve our understanding of galaxy evolution, and constrain the duration of reionization. The small aperture telescopes will target the largest angular scales observable from Chile, mapping ≈ 10% of the sky to a white noise level of 2 μK-arcmin in combined 93 and 145 GHz bands, to measure the primordial tensor-to-scalar ratio, r, at a target level of σ(r)=0.003. The large aperture telescope will map ≈ 40% of the sky at arcminute angular resolution to an expected white noise level of 6 μK-arcmin in combined 93 and 145 GHz bands, overlapping with the majority of the Large Synoptic Survey Telescope sky region and partially with the Dark Energy Spectroscopic Instrument. With up to an order of magnitude lower polarization noise than maps from the Planck satellite, the high-resolution sky maps will constrain cosmological parameters derived from the damping tail, gravitational lensing of the microwave background, the primordial bispectrum, and the thermal and kinematic Sunyaev-Zel'dovich effects, and will aid in delensing the large-angle polarization signal to measure the tensor-to-scalar ratio. The survey will also provide a legacy catalog of 16,000 galaxy clusters and more than 20,000 extragalactic sources.}, number={02}, journal={Journal of Cosmology and Astroparticle Physics}, publisher={IOP Publishing}, author={Ade, Peter and Aguirre, James and Ahmed, Zeeshan and Aiola, Simone and Ali, Aamir and Alonso, David and Alvarez, Marcelo A. and Arnold, Kam and Ashton, Peter and Austermann, Jason and et al.}, year={2019}, month={Feb}, pages={056–056} }
@article{wagoner_flanagan_2018, title={Baseball Physics: A New Mechanics Lab}, volume={56}, ISSN={0031-921X}, url={http://dx.doi.org/10.1119/1.5033871}, DOI={10.1119/1.5033871}, abstractNote={The game of baseball provides an interesting laboratory for experimenting with mechanical phenomena (there are many good examples in The Physics Teacher, available on Professor Alan Nathan’s website, and discussed in Physics of Baseball & Softball). We have developed a lab, for an introductory-level physics course, that investigates many of these phenomena. The lab uses inexpensive, readily available equipment such as wooden baseball bats, baseballs, and actual Major League Baseball data. By the end of the lab, students have revisited many concepts they learned earlier in the semester and come away with an understanding of how to put seemingly disparate ideas together to analyze a fun sport.}, number={5}, journal={The Physics Teacher}, publisher={American Association of Physics Teachers (AAPT)}, author={Wagoner, Kasey and Flanagan, Daniel}, year={2018}, month={May}, pages={290–292} }
@article{wagoner_hynes_flanagan_2018, title={Interesting Guided-Inquiry Labs for a Large-Enrollment, Active Learning Physics II Course}, volume={56}, ISSN={0031-921X}, url={http://dx.doi.org/10.1119/1.5028243}, DOI={10.1119/1.5028243}, abstractNote={Introductory physics labs often focus on a series of common experiments intending to teach the student the measurement side of physics. While these experiments have the potential to be quite instructive, we observed that our students often consider them to be boring and monotonous, which often leads to them being uninstructive. To combat this, we have designed a series of labs with two major goals: the experiments should be relevant to the students’ world, and the labs should gently guide the students to develop the experimental process on their own. Meeting these goals is difficult, particularly in a course with large enrollment where labs are instructed by graduate students. We have had success meeting these goals in our classroom, where over the last decade our introductory physics course has transformed from a traditional, lecture-learning class to a flipped class based on the textbook Six Ideas that Shaped Physics. Here we describe the structure of the new labs we have designed to capitalize on our classroom success while overcoming the aforementioned difficulties. These new labs are more engaging and instructive for our introductory physics students.}, number={4}, journal={The Physics Teacher}, publisher={American Association of Physics Teachers (AAPT)}, author={Wagoner, Kasey and Hynes, K. Mairin and Flanagan, Daniel}, year={2018}, month={Apr}, pages={244–247} }
@article{salatino_pappas_henderson_newburgh_niemack_staggs_wagoner_2017, title={Optimization of Advanced ACTPol Transition Edge Sensor Bolometer Operation Using R(T,I) Transition Measurements}, volume={27}, ISSN={1051-8223 1558-2515 2378-7074}, url={http://dx.doi.org/10.1109/tasc.2017.2672687}, DOI={10.1109/tasc.2017.2672687}, abstractNote={In the current submm and mm cosmology experiments the focal planes are populated by kilopixel transition edge sensors (TESes). Varying incoming power load requires frequent rebiasing of the TESes through standard current–voltage (IV) acquisition. The time required to perform IVs on such large arrays and the resulting transient heating of the bath reduces the sky observation time. We explore a bias step method that significantly reduces the time required for the rebiasing process. This exploits the detectors' responses to the injection of a small square wave signal on top of the dc bias current and knowledge of the shape of the detector transition R(T,I). This method has been tested on two detector arrays of the Atacama Cosmology Telescope (ACT). In this paper, we focus on the first step of the method, the estimate of the TES %Rn}, number={4}, journal={IEEE Transactions on Applied Superconductivity}, publisher={Institute of Electrical and Electronics Engineers (IEEE)}, author={Salatino, Maria and Pappas, Christine G. and Henderson, Shawn W. H. and Newburgh, Laura and Niemack, Michael D. and Staggs, Suzanne T. and Wagoner, Kasey}, year={2017}, month={Jun}, pages={1–6} }
@article{madziwa-nussinov_wagoner_shore_hutt_evans_krishnan_cowsik_2012, title={Characteristics and Response of a Rotational Seismometer to Seismic Signals}, volume={102}, ISSN={0037-1106}, url={http://dx.doi.org/10.1785/0120110166}, DOI={10.1785/0120110166}, abstractNote={A rotational seismometer capable of in situ measurements of rotational oscillations and tilts has been developed and calibrated. Its sensitivity to rotations and tilts at frequencies above 10 mHz is ![Graphic][1] , and this meets the recommendations of the International Working Group on Rotational Seismology (IWGoRS) for instrumental sensitivities for rotational seismology in the near field and for engineering applications. The design and calibration of this instrument and its frequency‐response function are presented, along with the signals initiated by an earthquake at a distance of ∼120 km. Finally, the steps we are taking to build a field instrument based on the experience gained with this engineering model are briefly discussed.
[1]: /embed/inline-graphic-1.gif}, number={2}, journal={Bulletin of the Seismological Society of America}, publisher={Seismological Society of America (SSA)}, author={Madziwa-Nussinov, T. and Wagoner, K. and Shore, P. and Hutt, C. R. and Evans, J. R. and Krishnan, N. and Cowsik, R.}, year={2012}, month={Mar}, pages={563–573} }
@phdthesis{wagoner_2010, place={St. Louis, MO}, title={Laboratory Investigations of Short Range Gravity}, school={Washington University in St. Louis}, author={Wagoner, K.}, year={2010}, month={Aug} }
@article{cowsik_wagoner_berti_sircar_2009, title={INTERNAL DYNAMICS AND DYNAMICAL FRICTION EFFECTS IN THE DWARF SPHEROIDAL GALAXY IN FORNAX}, volume={699}, ISSN={0004-637X 1538-4357}, url={http://dx.doi.org/10.1088/0004-637x/699/2/1389}, DOI={10.1088/0004-637x/699/2/1389}, abstractNote={In the Fornax dwarf spheroidal galaxy the globular clusters are distributed widely, without any significant central concentration. Oh et al. pointed out that such a distribution is paradoxical: dynamical friction effects estimated using single-component King models would have forced the globular clusters to spiral down to the center of the galaxy well within a Hubble time. This paper is devoted to a discussion of this paradox. We describe a model in which the stars of the dwarf spheroidal galaxy are embedded in a cloud of dark matter, and each of these components is specified by its own phase-space distribution function. This model allows us to fit self-consistently the observed luminosity profile and the spatial variation of the velocity dispersion of the stars. This fitting yields two basic parameters, related to the central density and velocity dispersion, that characterize the phase-space distribution of dark matter. The dynamical friction effects calculated on the basis of this self-consistent model are small enough that the observed spatial distribution of the globular clusters poses no difficulty, and the apparent paradox is resolved. Thus, we have at hand a model for Fornax that reproduces the main observed features of this dwarf spheroidal galaxy.}, number={2}, journal={The Astrophysical Journal}, publisher={American Astronomical Society}, author={Cowsik, Ramanath and Wagoner, Kasey and Berti, Emanuele and Sircar, Amit}, year={2009}, month={Jun}, pages={1389–1394} }
@article{cowsik_madziwa-nussinov_wagoner_wiens_wysession_2009, title={Performance Characteristics of a Rotational Seismometer for Near-Field and Engineering Applications}, volume={99}, ISSN={0037-1106}, url={http://dx.doi.org/10.1785/0120080207}, DOI={10.1785/0120080207}, abstractNote={Based on the concept that torsion balances act as good filters for rota- tional oscillations at frequencies above their natural frequency of oscillations, we have fabricated a simple prototype to serve as a rotational seismometer for near-field and engineering studies. This instrument displays a nearly flat response at frequencies above 10 mHz, and the preliminary data taken with this instrument show a sensitivity of 5 ! 10 ! 6 " ! =0:01 Hz# rad sec ! 1 Hz ! 1=2 . Marginal improvements of the fabrication and housing will be needed to fully cover the sensitivities recommended by a U.S. Geological Survey (USGS) panel for studies at these frequencies.}, number={2B}, journal={Bulletin of the Seismological Society of America}, publisher={Seismological Society of America (SSA)}, author={Cowsik, R. and Madziwa-Nussinov, T. and Wagoner, K. and Wiens, D. and Wysession, M.}, year={2009}, month={May}, pages={1181–1189} }
@article{cowsik_srinivasan_kasturirengan_kumar_wagoner_2007, title={Design and performance of a sub-nanoradian resolution autocollimating optical lever}, volume={78}, ISSN={0034-6748 1089-7623}, url={http://dx.doi.org/10.1063/1.2714044}, DOI={10.1063/1.2714044}, abstractNote={Precision goniometry using optics has the advantage that it does not impose much stress on the object of investigation and, as such, is adopted extensively in gravitational wave detection, in torsion balances investigating fundamental forces, in specialized studies of biological samples, and it has potential applications in condensed matter physics. In this article we present the considerations that go into designing optical levers and discuss the performance of the instrument we have constructed. We motivate the design by considering an idealized setup and the limitations to the angular resolution induced by statistical fluctuations of the photon count rate and diffraction at the apertures. The effects of digitization of the count rate and of the spatial location of the photons on the image plane motivating the actual design are discussed next. Based on these considerations, we have developed an autocollimating optical lever which has a very high resolution and dynamic range. An array of 110 slits, of 90 μm width and a pitch of 182 μm, is located in the focal plane of a field lens, of focal length 1000 mm, and is illuminated by a CCFL tube. This array is imaged back onto the focal plane after retroreflection from a mirror placed just beyond the lens. The image is recorded on a linear charge-coupled device array at the rate of 1000 images/s and is processed through a special algorithm to obtain the centroid. The instrument has a centroid stability of ∼3×10−10 rad Hz−1∕2 and a dynamic range of ∼107.}, number={3}, journal={Review of Scientific Instruments}, publisher={AIP Publishing}, author={Cowsik, R. and Srinivasan, R. and Kasturirengan, S. and Kumar, A. Senthil and Wagoner, K.}, year={2007}, month={Mar}, pages={035105} }