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1. ASKAP reveals the radio tail structure of the Corkscrew Galaxy shaped by its passage through the Abell 3627 cluster

Author

Koribalski, Bärbel S., Duchesne, Stefan W., Lenc, Emil, Venturi, Tiziana, Botteon, Andrea, Shabala, Stanislav S., Vernstrom, Tessa, Carretti, Ettore, Norris, Ray P., Anderson, Craig, Hopkins, Andrew M., Riseley, C. J., Gupta, Nikhel, and Velović, Velibor

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Among the bent tail radio galaxies common in galaxy clusters are some with long, collimated tails (so-called head-tail galaxies) shaped by their interactions with the intracluster medium (ICM). Here we report the discovery of intricate filamentary structure in and beyond the ~28' (570 kpc) long, helical radio tail of the Corkscrew Galaxy (1610-60.5, ESO137-G007), which resides in the X-ray bright cluster Abell 3627 (D = 70 Mpc). Deep radio continuum data were obtained with wide-field Phased Array Feeds on the Australian Square Kilometer Array Pathfinder (ASKAP) at 944 MHz and 1.4 GHz. The Corkscrew Galaxy is located 15' north of the prominent wide-angle tail (WAT) radio galaxy 1610-60.8 (ESO137-G006) near the cluster centre. While the bright (young) part of its radio tail is highly collimated, the faint (old) part shows increasing oscillation amplitudes, break-ups, and filaments. We find a stunning set of arc-shaped radio filaments beyond and mostly orthogonal to the collimated Corkscrew tail end, forming a partial bubble. This may be the first detection of a "proto-lobe" seen in 3D MHD simulations by Nolting et al. (2019), formed by the face-on impact of the Corkscrew Galaxy with a shock front in the cluster outskirts. Interactions of the radio galaxy tail with the ICM are likely responsible for the tail collimation and shear forces within the ICM for its increasingly filamentary structure. We also report the discovery of small (~20-30 kpc) ram-pressure stripped radio tails in four Abell 3627 cluster galaxies., Comment: 11 pages, 7 figures, MNRAS, submitted

Published
2024

2. The Physalis system: Discovery of ORC-like radio shells around a massive pair of interacting early-type galaxies with offset X-ray emission

Author

Koribalski, Bärbel S., Khabibullin, Ildar, Dolag, Klaus, Churazov, Eugene, Norris, Ray P., Carretti, Ettore, Hopkins, Andrew M., Vernstrom, Tessa, Shabala, Stanislav S., and Gupta, Nikhel

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the discovery of large radio shells around a massive pair of interacting galaxies and extended diffuse X-ray emission within the shells. The radio data were obtained with the Australian Square Kilometer Array Pathfinder (ASKAP) in two frequency bands centred at 944 MHz and 1.4 GHz, respectively, while the X-ray data are from the XMM-Newton observatory. The host galaxy pair, which consists of the early-type galaxies ESO 184-G042 and LEDA 418116, is part of a loose group at a distance of only 75 Mpc (redshift z = 0.017). The observed outer radio shells (diameter ~ 145 kpc) and ridge-like central emission of the system, ASKAP J1914-5433 (Physalis), are likely associated with merger shocks during the formation of the central galaxy (ESO 184-G042) and resemble the new class of odd radio circles (ORCs). This is supported by the brightest X-ray emission found offset from the centre of the Physalis system, instead centered at the less massive galaxy, LEDA 418116. The host galaxy pair is embedded in an irregular envelope of diffuse light, highlighting on-going interactions. We complement our combined radio and X-ray study with high-resolution simulations of the circumgalactic medium (CGM) around galaxy mergers from the Magneticum project to analyse the evolutionary state of the Physalis system. We argue that ORCs / radio shells could be produced by a combination of energy release from the central AGN and subsequent lightening up in radio emission by merger shocks traveling through the CGM of these systems., Comment: 12 pages, 8 figures, submitted to MNRAS

Published
2024

3. RG-CAT: Detection Pipeline and Catalogue of Radio Galaxies in the EMU Pilot Survey

Author

Gupta, Nikhel, Norris, Ray P., Hayder, Zeeshan, Huynh, Minh, Petersson, Lars, Wang, X. Rosalind, Hopkins, Andrew M., Andernach, Heinz, Gordon, Yjan, Riggi, Simone, Yew, Miranda, Crawford, Evan J., Koribalski, Bärbel, Filipović, Miroslav D., Kapinśka, Anna D., Shabala, Stanislav, Vernstrom, Tessa, and Marvil, Joshua R.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Computer Science - Computer Vision and Pattern Recognition, Computer Science - Machine Learning
Abstract

We present source detection and catalogue construction pipelines to build the first catalogue of radio galaxies from the 270 $\rm deg^2$ pilot survey of the Evolutionary Map of the Universe (EMU-PS) conducted with the Australian Square Kilometre Array Pathfinder (ASKAP) telescope. The detection pipeline uses Gal-DINO computer-vision networks (Gupta et al., 2024) to predict the categories of radio morphology and bounding boxes for radio sources, as well as their potential infrared host positions. The Gal-DINO network is trained and evaluated on approximately 5,000 visually inspected radio galaxies and their infrared hosts, encompassing both compact and extended radio morphologies. We find that the Intersection over Union (IoU) for the predicted and ground truth bounding boxes is larger than 0.5 for 99% of the radio sources, and 98% of predicted host positions are within $3^{\prime \prime}$ of the ground truth infrared host in the evaluation set. The catalogue construction pipeline uses the predictions of the trained network on the radio and infrared image cutouts based on the catalogue of radio components identified using the Selavy source finder algorithm. Confidence scores of the predictions are then used to prioritize Selavy components with higher scores and incorporate them first into the catalogue. This results in identifications for a total of 211,625 radio sources, with 201,211 classified as compact and unresolved. The remaining 10,414 are categorized as extended radio morphologies, including 582 FR-I, 5,602 FR-II, 1,494 FR-x (uncertain whether FR-I or FR-II), 2,375 R (single-peak resolved) radio galaxies, and 361 with peculiar and other rare morphologies. We cross-match the radio sources in the catalogue with the infrared and optical catalogues, finding infrared cross-matches for 73% and photometric redshifts for 36% of the radio galaxies., Comment: Accepted for publication in PASA. The paper has 22 pages, 12 figures and 5 tables

Published
2024

4. A Multimodal Dataset and Benchmark for Radio Galaxy and Infrared Host Detection

Author

Gupta, Nikhel, Hayder, Zeeshan, Norris, Ray P., Hyunh, Minh, and Petersson, Lars

Subjects
Computer Science - Computer Vision and Pattern Recognition, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We present a novel multimodal dataset developed by expert astronomers to automate the detection and localisation of multi-component extended radio galaxies and their corresponding infrared hosts. The dataset comprises 4,155 instances of galaxies in 2,800 images with both radio and infrared modalities. Each instance contains information on the extended radio galaxy class, its corresponding bounding box that encompasses all of its components, pixel-level segmentation mask, and the position of its corresponding infrared host galaxy. Our dataset is the first publicly accessible dataset that includes images from a highly sensitive radio telescope, infrared satellite, and instance-level annotations for their identification. We benchmark several object detection algorithms on the dataset and propose a novel multimodal approach to identify radio galaxies and the positions of infrared hosts simultaneously., Comment: Accepted in NeurIPS 2023 conference ML4PS workshop (https://nips.cc/). The full version accepted in PASA, is available at https://doi.org/10.1017/pasa.2023.64

Published
2023
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5. RadioGalaxyNET: Dataset and Novel Computer Vision Algorithms for the Detection of Extended Radio Galaxies and Infrared Hosts

Author

Gupta, Nikhel, Hayder, Zeeshan, Norris, Ray P., Huynh, Minh, and Petersson, Lars

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Computer Science - Computer Vision and Pattern Recognition
Abstract

Creating radio galaxy catalogues from next-generation deep surveys requires automated identification of associated components of extended sources and their corresponding infrared hosts. In this paper, we introduce RadioGalaxyNET, a multimodal dataset, and a suite of novel computer vision algorithms designed to automate the detection and localization of multi-component extended radio galaxies and their corresponding infrared hosts. The dataset comprises 4,155 instances of galaxies in 2,800 images with both radio and infrared channels. Each instance provides information about the extended radio galaxy class, its corresponding bounding box encompassing all components, the pixel-level segmentation mask, and the keypoint position of its corresponding infrared host galaxy. RadioGalaxyNET is the first dataset to include images from the highly sensitive Australian Square Kilometre Array Pathfinder (ASKAP) radio telescope, corresponding infrared images, and instance-level annotations for galaxy detection. We benchmark several object detection algorithms on the dataset and propose a novel multimodal approach to simultaneously detect radio galaxies and the positions of infrared hosts., Comment: Accepted for publication in PASA. The paper has 17 pages, 6 figures, 5 tables

Published
2023

6. Deep Learning for Morphological Identification of Extended Radio Galaxies using Weak Labels

Author

Gupta, Nikhel, Hayder, Zeeshan, Norris, Ray P., Huynh, Minh, Petersson, Lars, Wang, X. Rosalind, Andernach, Heinz, Koribalski, Bärbel S., Yew, Miranda, and Crawford, Evan J.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Computer Science - Computer Vision and Pattern Recognition, Computer Science - Machine Learning
Abstract

The present work discusses the use of a weakly-supervised deep learning algorithm that reduces the cost of labelling pixel-level masks for complex radio galaxies with multiple components. The algorithm is trained on weak class-level labels of radio galaxies to get class activation maps (CAMs). The CAMs are further refined using an inter-pixel relations network (IRNet) to get instance segmentation masks over radio galaxies and the positions of their infrared hosts. We use data from the Australian Square Kilometre Array Pathfinder (ASKAP) telescope, specifically the Evolutionary Map of the Universe (EMU) Pilot Survey, which covered a sky area of 270 square degrees with an RMS sensitivity of 25-35 $\mu$Jy/beam. We demonstrate that weakly-supervised deep learning algorithms can achieve high accuracy in predicting pixel-level information, including masks for the extended radio emission encapsulating all galaxy components and the positions of the infrared host galaxies. We evaluate the performance of our method using mean Average Precision (mAP) across multiple classes at a standard intersection over union (IoU) threshold of 0.5. We show that the model achieves a mAP$_{50}$ of 67.5\% and 76.8\% for radio masks and infrared host positions, respectively. The network architecture can be found at the following link: https://github.com/Nikhel1/Gal-CAM, Comment: 14 pages, 6 figues, accepted for publication in PASA

Published
2023

7. Discovery of Peculiar Radio Morphologies with ASKAP using Unsupervised Machine Learning

Author

Gupta, Nikhel, Huynh, Minh, Norris, Ray P., Wang, Rosalind, Hopkins, Andrew M., Andernach, Heinz, Koribalski, Bärbel S., and Galvin, Tim J.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We present a set of peculiar radio sources detected using an unsupervised machine learning method. We use data from the Australian Square Kilometre Array Pathfinder (ASKAP) telescope to train a self-organizing map (SOM). The radio maps from three ASKAP surveys, Evolutionary Map of Universe pilot survey (EMU-PS), Deep Investigation of Neutral Gas Origins pilot survey (DINGO) and Survey With ASKAP of GAMA-09 + X-ray (SWAG-X), are used to search for the rarest or unknown radio morphologies. We use an extension of the SOM algorithm that implements rotation and flipping invariance on astronomical sources. The SOM is trained using the images of all "complex" radio sources in the EMU-PS which we define as all sources catalogued as "multi-component". The trained SOM is then used to estimate a similarity score for complex sources in all surveys. We select 0.5\% of the sources that are most complex according to the similarity metric, and visually examine them to find the rarest radio morphologies. Among these, we find two new odd radio circle (ORC) candidates and five other peculiar morphologies. We discuss multiwavelength properties and the optical/infrared counterparts of selected peculiar sources. In addition, we present examples of conventional radio morphologies including: diffuse emission from galaxy clusters, and resolved, bent-tailed, and FR-I and FR-II type radio galaxies. We discuss the overdense environment that may be the reason behind the circular shape of ORC candidates., Comment: Accepted in PASA, 23 pages, 16 figures

Published
2022
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8. CMB-S4: Forecasting Constraints on Primordial Gravitational Waves

Author

Abazajian, Kevork, Addison, Graeme E, Adshead, Peter, Ahmed, Zeeshan, Akerib, Daniel, Ali, Aamir, Allen, Steven W, Alonso, David, Alvarez, Marcelo, Amin, Mustafa A, Anderson, Adam, Arnold, Kam S, Ashton, Peter, Baccigalupi, Carlo, Bard, Debbie, Barkats, Denis, Barron, Darcy, Barry, Peter S, Bartlett, James G, Thakur, Ritoban Basu, Battaglia, Nicholas, Bean, Rachel, Bebek, Chris, Bender, Amy N, Benson, Bradford A, Bianchini, Federico, Bischoff, Colin A, Bleem, Lindsey, Bock, James J, Bocquet, Sebastian, Boddy, Kimberly K, Bond, J Richard, Borrill, Julian, Bouchet, François R, Brinckmann, Thejs, Brown, Michael L, Bryan, Sean, Buza, Victor, Byrum, Karen, Caimapo, Carlos Hervias, Calabrese, Erminia, Calafut, Victoria, Caldwell, Robert, Carlstrom, John E, Carron, Julien, Cecil, Thomas, Challinor, Anthony, Chang, Clarence L, Chinone, Yuji, Cho, Hsiao-Mei Sherry, Cooray, Asantha, Coulton, Will, Crawford, Thomas M, Crites, Abigail, Cukierman, Ari, Cyr-Racine, Francis-Yan, de Haan, Tijmen, Delabrouille, Jacques, Devlin, Mark, Di Valentino, Eleonora, Dierickx, Marion, Dobbs, Matt, Duff, Shannon, Dvorkin, Cora, Eimer, Joseph, Elleflot, Tucker, Errard, Josquin, Essinger-Hileman, Thomas, Fabbian, Giulio, Feng, Chang, Ferraro, Simone, Filippini, Jeffrey P, Flauger, Raphael, Flaugher, Brenna, Fraisse, Aurelien A, Frolov, Andrei, Galitzki, Nicholas, Gallardo, Patricio A, Galli, Silvia, Ganga, Ken, Gerbino, Martina, Gluscevic, Vera, Goeckner-Wald, Neil, Green, Daniel, Grin, Daniel, Grohs, Evan, Gualtieri, Riccardo, Gudmundsson, Jon E, Gullett, Ian, Gupta, Nikhel, Habib, Salman, Halpern, Mark, Halverson, Nils W, Hanany, Shaul, Harrington, Kathleen, Hasegawa, Masaya, Hasselfield, Matthew, Hazumi, Masashi, Heitmann, Katrin, and Henderson, Shawn

Subjects
Particle and High Energy Physics, Physical Sciences, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

CMB-S4 - the next-generation ground-based cosmic microwave background (CMB) experiment - is set to significantly advance the sensitivity of CMB measurements and enhance our understanding of the origin and evolution of the universe. Among the science cases pursued with CMB-S4, the quest for detecting primordial gravitational waves is a central driver of the experimental design. This work details the development of a forecasting framework that includes a power-spectrum-based semianalytic projection tool, targeted explicitly toward optimizing constraints on the tensor-to-scalar ratio, r, in the presence of Galactic foregrounds and gravitational lensing of the CMB. This framework is unique in its direct use of information from the achieved performance of current Stage 2-3 CMB experiments to robustly forecast the science reach of upcoming CMB-polarization endeavors. The methodology allows for rapid iteration over experimental configurations and offers a flexible way to optimize the design of future experiments, given a desired scientific goal. To form a closed-loop process, we couple this semianalytic tool with map-based validation studies, which allow for the injection of additional complexity and verification of our forecasts with several independent analysis methods. We document multiple rounds of forecasts for CMB-S4 using this process and the resulting establishment of the current reference design of the primordial gravitational-wave component of the Stage-4 experiment, optimized to achieve our science goals of detecting primordial gravitational waves for r > 0.003 at greater than 5σ, or in the absence of a detection, of reaching an upper limit of r < 0.001 at 95% CL.

Published
2022

9. CMB-S4: Forecasting Constraints on Primordial Gravitational Waves

Author

Collaboration, CMB-S4, Abazajian, Kevork, Addison, Graeme E., Adshead, Peter, Ahmed, Zeeshan, Akerib, Daniel, Ali, Aamir, Allen, Steven W., Alonso, David, Alvarez, Marcelo, Amin, Mustafa A., Anderson, Adam, Arnold, Kam S., Ashton, Peter, Baccigalupi, Carlo, Bard, Debbie, Barkats, Denis, Barron, Darcy, Barry, Peter S., Bartlett, James G., Thakur, Ritoban Basu, Battaglia, Nicholas, Bean, Rachel, Bebek, Chris, Bender, Amy N., Benson, Bradford A., Bianchini, Federico, Bischoff, Colin A., Bleem, Lindsey, Bock, James J., Bocquet, Sebastian, Boddy, Kimberly K., Bond, J. Richard, Borrill, Julian, Bouchet, François R., Brinckmann, Thejs, Brown, Michael L., Bryan, Sean, Buza, Victor, Byrum, Karen, Caimapo, Carlos Hervias, Calabrese, Erminia, Calafut, Victoria, Caldwell, Robert, Carlstrom, John E., Carron, Julien, Cecil, Thomas, Challinor, Anthony, Chang, Clarence L., Chinone, Yuji, Cho, Hsiao-Mei Sherry, Cooray, Asantha, Coulton, Will, Crawford, Thomas M., Crites, Abigail, Cukierman, Ari, Cyr-Racine, Francis-Yan, de Haan, Tijmen, Delabrouille, Jacques, Devlin, Mark, Di Valentino, Eleonora, Dierickx, Marion, Dobbs, Matt, Duff, Shannon, Dunkley, Jo, Dvorkin, Cora, Eimer, Joseph, Elleflot, Tucker, Errard, Josquin, Essinger-Hileman, Thomas, Fabbian, Giulio, Feng, Chang, Ferraro, Simone, Filippini, Jeffrey P., Flauger, Raphael, Flaugher, Brenna, Fraisse, Aurelien A., Frolov, Andrei, Galitzki, Nicholas, Gallardo, Patricio A., Galli, Silvia, Ganga, Ken, Gerbino, Martina, Gluscevic, Vera, Goeckner-Wald, Neil, Green, Daniel, Grin, Daniel, Grohs, Evan, Gualtieri, Riccardo, Gudmundsson, Jon E., Gullett, Ian, Gupta, Nikhel, Habib, Salman, Halpern, Mark, Halverson, Nils W., Hanany, Shaul, Harrington, Kathleen, Hasegawa, Masaya, Hasselfield, Matthew, Hazumi, Masashi, Heitmann, Katrin, Henderson, Shawn, Hensley, Brandon, Hill, Charles, Hill, J. Colin, Hlozek, Renée, Ho, Shuay-Pwu Patty, Hoang, Thuong, Holder, Gil, Holzapfel, William, Hood, John, Hubmayr, Johannes, Huffenberger, Kevin M., Hui, Howard, Irwin, Kent, Jeong, Oliver, Johnson, Bradley R., Jones, William C., Kang, Jae Hwan, Karkare, Kirit S., Katayama, Nobuhiko, Keskitalo, Reijo, Kisner, Theodore, Knox, Lloyd, Koopman, Brian J., Kosowsky, Arthur, Kovac, John, Kovetz, Ely D., Kuhlmann, Steve, Kuo, Chao-lin, Kusaka, Akito, Lähteenmäki, Anne, Lawrence, Charles R., Lee, Adrian T., Lewis, Antony, Li, Dale, Linder, Eric, Loverde, Marilena, Lowitz, Amy, Lubin, Phil, Madhavacheril, Mathew S., Mantz, Adam, Marques, Gabriela, Matsuda, Frederick, Mauskopf, Philip, McCarrick, Heather, McMahon, Jeffrey, Meerburg, P. Daniel, Melin, Jean-Baptiste, Menanteau, Felipe, Meyers, Joel, Millea, Marius, Mohr, Joseph, Moncelsi, Lorenzo, Monzani, Maria, Mroczkowski, Tony, Mukherjee, Suvodip, Nagy, Johanna, Namikawa, Toshiya, Nati, Federico, Natoli, Tyler, Newburgh, Laura, Niemack, Michael D., Nishino, Haruki, Nord, Brian, Novosad, Valentine, O'Brient, Roger, Padin, Stephen, Palladino, Steven, Partridge, Bruce, Petravick, Don, Pierpaoli, Elena, Pogosian, Levon, Prabhu, Karthik, Pryke, Clement, Puglisi, Giuseppe, Racine, Benjamin, Rahlin, Alexandra, Rao, Mayuri Sathyanarayana, Raveri, Marco, Reichardt, Christian L., Remazeilles, Mathieu, Rocha, Graca, Roe, Natalie A., Roy, Anirban, Ruhl, John E., Salatino, Maria, Saliwanchik, Benjamin, Schaan, Emmanuel, Schillaci, Alessandro, Schmitt, Benjamin, Schmittfull, Marcel M., Scott, Douglas, Sehgal, Neelima, Shandera, Sarah, Sherwin, Blake D., Shirokoff, Erik, Simon, Sara M., Slosar, Anze, Spergel, David, Germaine, Tyler St., Staggs, Suzanne T., Stark, Antony, Starkman, Glenn D., Stompor, Radek, Stoughton, Chris, Suzuki, Aritoki, Tajima, Osamu, Teply, Grant P., Thompson, Keith, Thorne, Ben, Timbie, Peter, Tomasi, Maurizio, Tristram, Matthieu, Tucker, Gregory, Umiltà, Caterina, van Engelen, Alexander, Vavagiakis, Eve M., Vieira, Joaquin D., Vieregg, Abigail G., Wagoner, Kasey, Wallisch, Benjamin, Wang, Gensheng, Watson, Scott, Westbrook, Ben, Whitehorn, Nathan, Wollack, Edward J., Wu, W. L. Kimmy, Xu, Zhilei, Yang, H. Y. Eric, Yasini, Siavash, Yefremenko, Volodymyr G., Yoon, Ki Won, Young, Edward, Yu, Cyndia, and Zonca, Andrea

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

CMB-S4---the next-generation ground-based cosmic microwave background (CMB) experiment---is set to significantly advance the sensitivity of CMB measurements and enhance our understanding of the origin and evolution of the Universe, from the highest energies at the dawn of time through the growth of structure to the present day. Among the science cases pursued with CMB-S4, the quest for detecting primordial gravitational waves is a central driver of the experimental design. This work details the development of a forecasting framework that includes a power-spectrum-based semi-analytic projection tool, targeted explicitly towards optimizing constraints on the tensor-to-scalar ratio, $r$, in the presence of Galactic foregrounds and gravitational lensing of the CMB. This framework is unique in its direct use of information from the achieved performance of current Stage 2--3 CMB experiments to robustly forecast the science reach of upcoming CMB-polarization endeavors. The methodology allows for rapid iteration over experimental configurations and offers a flexible way to optimize the design of future experiments given a desired scientific goal. To form a closed-loop process, we couple this semi-analytic tool with map-based validation studies, which allow for the injection of additional complexity and verification of our forecasts with several independent analysis methods. We document multiple rounds of forecasts for CMB-S4 using this process and the resulting establishment of the current reference design of the primordial gravitational-wave component of the Stage-4 experiment, optimized to achieve our science goals of detecting primordial gravitational waves for $r > 0.003$ at greater than $5\sigma$, or, in the absence of a detection, of reaching an upper limit of $r < 0.001$ at $95\%$ CL., Comment: 24 pages, 8 figures, 9 tables, submitted to ApJ. arXiv admin note: text overlap with arXiv:1907.04473

Published
2020
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10. Forecasts for Next Generation tSZ Surveys: the Impact of a Cosmology-Dependent Selection Function

Author

Gupta, Nikhel, Porciani, Cristiano, and Basu, Kaustuv

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The thermal Sunyaev-Zel'dovich (tSZ) effect is one of the primary tools for finding and characterizing galaxy clusters. Several ground-based experiments are either underway or are being planned for mapping wide areas of the sky at $\sim 150$ GHz with large-aperture telescopes. We present cosmological forecasts for a 'straw man' tSZ survey that will observe a sky area between $200$ and $10^4$ deg$^2$ to an rms noise level between 2.8 and 20.2 $\mu$K-arcmin. The probes we consider are the cluster number counts (as a function of the integrated Compton-$Y$ parameter and redshift) and their angular clustering (as a function of redshift). At fixed observing time, we find that wider surveys constrain cosmology slightly better than deeper ones due to their increased ability to detect rare high-mass clusters. In all cases, we notice that adding the clustering information does not practically improve the constraints derived from the number counts. We compare forecasts obtained by sampling the posterior distribution with the Markov-chain-Monte-Carlo method against those derived using the Fisher-matrix formalism. We find that the latter produces slightly optimistic constraints where errors are underestimated at the 10 per cent level. Most importantly, we use an analytic method to estimate the selection function of the survey and account for its response to variations of the cosmological parameters in the likelihood function. Our analysis demonstrates that neglecting this effect (as routinely done in the literature) yields artificially tighter constraints by a factor of 2.2 and 1.7 for $\sigma_8$ and $\Omega_\mathrm{M}$, respectively., Comment: 12 pages, 9 figures

Published
2020

11. Mass Estimation of Galaxy Clusters with Deep Learning I: Sunyaev-Zel'dovich Effect

Author

Gupta, Nikhel and Reichardt, Christian L.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Computer Science - Machine Learning
Abstract

We present a new application of deep learning to infer the masses of galaxy clusters directly from images of the microwave sky. Effectively, this is a novel approach to determining the scaling relation between a cluster's Sunyaev-Zel'dovich (SZ) effect signal and mass. The deep learning algorithm used is mResUNet, which is a modified feed-forward deep learning algorithm that broadly combines residual learning, convolution layers with different dilation rates, image regression activation and a U-Net framework. We train and test the deep learning model using simulated images of the microwave sky that include signals from the cosmic microwave background (CMB), dusty and radio galaxies, instrumental noise as well as the cluster's own SZ signal. The simulated cluster sample covers the mass range 1$\times 10^{14}~\rm M_{\odot}$ $

Published
2020

12. Discovery of a Powerful >10^61 erg AGN Outburst in Distant Galaxy Cluster SPT-CLJ0528-5300

Author

Calzadilla, Michael S., McDonald, Michael, Bayliss, Matthew, Benson, Bradford A., Bleem, Lindsey E., Brodwin, Mark, Edge, Alastair C., Floyd, Benjamin, Gupta, Nikhel, Hlavacek-Larrondo, Julie, McNamara, Brian R., and Reichardt, Christian L.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present ~103 ks of Chandra observations of the galaxy cluster SPT-CLJ0528-5300 (SPT0528, z=0.768). This cluster harbors the most radio-loud (L_1.4GHz = 1.01 x 10^33 erg/s/Hz) central AGN of any cluster in the South Pole Telescope (SPT) SZ survey with available X-ray data. We find evidence of AGN-inflated cavities in the X-ray emission, which are consistent with the orientation of the jet direction revealed by ATCA radio data. The combined probability that two such depressions -- each at ~1.4-1.8sigma significance, oriented ~180 degrees apart and aligned with the jet axis -- would occur by chance is 0.1%. At >10^61 erg, the outburst in SPT0528 is among the most energetic known in the universe, and certainly the most powerful known at z>0.25. This work demonstrates that such powerful outbursts can be detected even in shallow X-ray exposures out to relatively high redshifts (z~0.8), providing an avenue for studying the evolution of extreme AGN feedback. The ratio of the cavity power (P_cav = 9.4+/-5.8 x 10^45 erg/s) to the cooling luminosity (L_cool = 1.5+/-0.5 x 10^44 erg/s) for SPT0528 is among the highest measured to date. If, in the future, additional systems are discovered at similar redshifts with equally high P_cav/L_cool ratios, it would imply that the feedback/cooling cycle was not as gentle at high redshifts as in the low-redshift universe., Comment: Accepted to ApJL. 8 pages, 5 figures

Published
2019
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13. The Massive and Distant Clusters of WISE Survey VI: Stellar Mass Fractions of a Sample of High-Redshift Infrared-selected Clusters

Author

Decker, Bandon, Brodwin, Mark, Abdulla, Zubair, Gonzalez, Anthony H., Marrone, Daniel P., O'Donnell, Christine, Stanford, S. A., Wylezalek, Dominika, Carlstrom, John E., Eisenhardt, Peter R. M., Mantz, Adam, Mo, Wenli, Moravec, Emily, Stern, Daniel, Aldering, Greg, Ashby, Matthew L. N., Boone, Kyle, Hayden, Brian, Gupta, Nikhel, and McDonald, Michael A.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present measurements of the stellar mass fractions ($f_\star$) for a sample of high-redshift ($0.93 \le z \le 1.32$) infrared-selected galaxy clusters from the Massive and Distant Clusters of WISE Survey (MaDCoWS) and compare them to the stellar mass fractions of Sunyaev-Zel'dovich (SZ) effect-selected clusters in a similar mass and redshift range from the South Pole Telescope (SPT)-SZ Survey. We do not find a significant difference in mean $f_\star$ between the two selection methods, though we do find an unexpectedly large range in $f_\star$ for the SZ-selected clusters. In addition, we measure the luminosity function of the MaDCoWS clusters and find $m^*= 19.41\pm0.07$, similar to other studies of clusters at or near our redshift range. Finally, we present SZ detections and masses for seven MaDCoWS clusters and new spectroscopic redshifts for five MaDCoWS clusters. One of these new clusters, MOO J1521+0452 at $z=1.31$, is the most distant MaDCoWS cluster confirmed to date., Comment: Accepted to ApJ

Published
2019
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14. Primordial Non-Gaussianity

Author

Meerburg, P. Daniel, Green, Daniel, Abidi, Muntazir, Amin, Mustafa A., Adshead, Peter, Ahmed, Zeeshan, Alonso, David, Ansarinejad, Behzad, Armstrong, Robert, Avila, Santiago, Baccigalupi, Carlo, Baldauf, Tobias, Ballardini, Mario, Bandura, Kevin, Bartolo, Nicola, Battaglia, Nicholas, Baumann, Daniel, Bavdhankar, Chetan, Bernal, José Luis, Beutler, Florian, Biagetti, Matteo, Bischoff, Colin, Blazek, Jonathan, Bond, J. Richard, Borrill, Julian, Bouchet, François R., Bull, Philip, Burgess, Cliff, Byrnes, Christian, Calabrese, Erminia, Carlstrom, John E., Castorina, Emanuele, Challinor, Anthony, Chang, Tzu-Ching, Chaves-Montero, Jonas, Chen, Xingang, Yeche, Christophe, Cooray, Asantha, Coulton, William, Crawford, Thomas, Chisari, Elisa, Cyr-Racine, Francis-Yan, D'Amico, Guido, de Bernardis, Paolo, de la Macorra, Axel, Doré, Olivier, Duivenvoorden, Adri, Dunkley, Joanna, Dvorkin, Cora, Eggemeier, Alexander, Escoffier, Stephanie, Essinger-Hileman, Tom, Fasiello, Matteo, Ferraro, Simone, Flauger, Raphael, Font-Ribera, Andreu, Foreman, Simon, Friedrich, Oliver, Garcia-Bellido, Juan, Gerbino, Martina, Gluscevic, Vera, Goon, Garrett, Gorski, Krzysztof M., Gudmundsson, Jon E., Gupta, Nikhel, Hanany, Shaul, Handley, Will, Hawken, Adam J., Hill, J. Colin, Hirata, Christopher M., Hložek, Renée, Holder, Gilbert, Huterer, Dragan, Kamionkowski, Marc, Karkare, Kirit S., Keeley, Ryan E., Kinney, William, Kisner, Theodore, Kneib, Jean-Paul, Knox, Lloyd, Koushiappas, Savvas M., Kovetz, Ely D., Koyama, Kazuya, L'Huillier, Benjamin, Lahav, Ofer, Lattanzi, Massimiliano, Lee, Hayden, Liguori, Michele, Loverde, Marilena, Madhavacheril, Mathew, Maldacena, Juan, Marsh, M. C. David, Masui, Kiyoshi, Matarrese, Sabino, McAllister, Liam, McMahon, Jeff, McQuinn, Matthew, Meyers, Joel, Mirbabayi, Mehrdad, Dizgah, Azadeh Moradinezhad, Motloch, Pavel, Mukherjee, Suvodip, Muñoz, Julian B., Myers, Adam D., Nagy, Johanna, Naselsky, Pavel, Nati, Federico, Newburgh, Nicolis, Alberto, Niemack, Michael D., Niz, Gustavo, Nomerotski, Andrei, Page, Lyman, Pajer, Enrico, Padmanabhan, Hamsa, Palma, Gonzalo A., Peiris, Hiranya V., Percival, Will J., Piacentni, Francesco, Pimentel, Guilherme L., Pogosian, Levon, Prescod-Weinstein, Chanda, Pryke, Clement, Puglisi, Giuseppe, Racine, Benjamin, Stompor, Radek, Raveri, Marco, Remazeilles, Mathieu, Rocha, Gracca, Ross, Ashley J., Rossi, Graziano, Ruhl, John, Sasaki, Misao, Schaan, Emmanuel, Schillaci, Alessandro, Schmittfull, Marcel, Sehgal, Neelima, Senatore, Leonardo, Seo, Hee-Jong, Shan, Huanyuan, Shandera, Sarah, Sherwin, Blake D., Silverstein, Eva, Simon, Sara, Slosar, Anže, Staggs, Suzanne, Starkman, Glenn, Stebbins, Albert, Suzuki, Aritoki, Switzer, Eric R., Timbie, Peter, Tolley, Andrew J., Tomasi, Maurizio, Tristram, Matthieu, Trodden, Mark, Tsai, Yu-Dai, Uhlemann, Cora, Umilta, Caterina, van Engelen, Alexander, Vargas-Magaña, M., Vieregg, Abigail, Wallisch, Benjamin, Wands, David, Wandelt, Benjamin, Wang, Yi, Watson, Scott, Wise, Mark, Wu, W. L. K., Xianyu, Zhong-Zhi, Xu, Weishuang, Yasini, Siavash, Young, Sam, Yutong, Duan, Zaldarriaga, Matias, Zemcov, Michael, Zhao, Gong-Bo, Zheng, Yi, and Zhu, Ningfeng

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, High Energy Physics - Theory
Abstract

Our current understanding of the Universe is established through the pristine measurements of structure in the cosmic microwave background (CMB) and the distribution and shapes of galaxies tracing the large scale structure (LSS) of the Universe. One key ingredient that underlies cosmological observables is that the field that sources the observed structure is assumed to be initially Gaussian with high precision. Nevertheless, a minimal deviation from Gaussianityis perhaps the most robust theoretical prediction of models that explain the observed Universe; itis necessarily present even in the simplest scenarios. In addition, most inflationary models produce far higher levels of non-Gaussianity. Since non-Gaussianity directly probes the dynamics in the early Universe, a detection would present a monumental discovery in cosmology, providing clues about physics at energy scales as high as the GUT scale., Comment: 5 pages + references; Submitted to the Astro2020 call for science white papers. This version: fixed author list

Published
2019

15. Science from an Ultra-Deep, High-Resolution Millimeter-Wave Survey

Author

Sehgal, Neelima, Nguyen, Ho Nam, Meyers, Joel, Munchmeyer, Moritz, Mroczkowski, Tony, Di Mascolo, Luca, Baxter, Eric, Cyr-Racine, Francis-Yan, Madhavacheril, Mathew, Beringue, Benjamin, Holder, Gil, Nagai, Daisuke, Dicker, Simon, Dvorkin, Cora, Ferraro, Simone, Fuller, George M., Gluscevic, Vera, Han, Dongwon, Jain, Bhuvnesh, Johnson, Bradley, Klaassen, Pamela, Meerburg, Daan, Motloch, Pavel, Spergel, David N., van Engelen, Alexander, Adshead, Peter, Armstrong, Robert, Baccigalupi, Carlo, Barron, Darcy, Basu, Kaustuv, Benson, Bradford, Beutler, Florian, Bond, J. Richard, Borrill, Julian, Calabrese, Erminia, Darwish, Omar, Denny, S. Lucas, Douglass, Kelly A., Essinger-Hileman, Tom, Foreman, Simon, Frayer, David, Gerbino, Martina, Gontcho, Satya Gontcho A, Grohs, Evan B., Gupta, Nikhel, Hill, J. Colin, Hirata, Christopher M., Hotinli, Selim, Johnson, Matthew C., Kamionkowski, Marc, Kovetz, Ely D., Lau, Erwin T., Liguori, Michele, Namikawa, Toshiya, Newburgh, Laura, Partridge, Bruce, Piacentni, Francesco, Rose, Benjamin, Rossi, Graziano, Saliwanchik, Benjamin, Schaan, Emmanuel, Shan, Huanyuan, Simon, Sara, Slosar, Anže, Switzer, Eric R., Trac, Hy, Xu, Weishuang, Zaldarriaga, Matias, and Zemcov, Michael

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, High Energy Physics - Phenomenology
Abstract

Opening up a new window of millimeter-wave observations that span frequency bands in the range of 30 to 500 GHz, survey half the sky, and are both an order of magnitude deeper (about 0.5 uK-arcmin) and of higher-resolution (about 10 arcseconds) than currently funded surveys would yield an enormous gain in understanding of both fundamental physics and astrophysics. In particular, such a survey would allow for major advances in measuring the distribution of dark matter and gas on small-scales, and yield needed insight on 1.) dark matter particle properties, 2.) the evolution of gas and galaxies, 3.) new light particle species, 4.) the epoch of inflation, and 5.) the census of bodies orbiting in the outer Solar System., Comment: 5 pages + references; Submitted to the Astro2020 call for science white papers

Published
2019

16. CMB-S4: Forecasting Constraints on Primordial Gravitational Waves

Author

Collaboration, The CMB-S4, :, Abazajian, Kevork, Addison, Graeme E, Adshead, Peter, Ahmed, Zeeshan, Akerib, Daniel, Ali, Aamir, Allen, Steven W, Alonso, David, Alvarez, Marcelo, Amin, Mustafa A, Anderson, Adam, Arnold, Kam S, Ashton, Peter, Baccigalupi, Carlo, Bard, Debbie, Barkats, Denis, Barron, Darcy, Barry, Peter S, Bartlett, James G, Thakur, Ritoban Basu, Battaglia, Nicholas, Bean, Rachel, Bebek, Chris, Bender, Amy N, Benson, Bradford A, Bianchini, Federico, Bischoff, Colin A, Bleem, Lindsey, Bock, James J, Bocquet, Sebastian, Boddy, Kimberly K, Bond, J Richard, Borrill, Julian, Bouchet, François R, Brinckmann, Thejs, Brown, Michael L, Bryan, Sean, Buza, Victor, Byrum, Karen, Caimapo, Carlos Hervias, Calabrese, Erminia, Calafut, Victoria, Caldwell, Robert, Carlstrom, John E, Carron, Julien, Cecil, Thomas, Challinor, Anthony, Chang, Clarence L, Chinone, Yuji, Cho, Hsiao-Mei Sherry, Cooray, Asantha, Coulton, Will, Crawford, Thomas M, Crites, Abigail, Cukierman, Ari, Cyr-Racine, Francis-Yan, de Haan, Tijmen, Delabrouille, Jacques, Devlin, Mark, Di Valentino, Eleonora, Dierickx, Marion, Dobbs, Matt, Duff, Shannon, Dunkley, Jo, Dvorkin, Cora, Eimer, Joseph, Elleflot, Tucker, Errard, Josquin, Essinger-Hileman, Thomas, Fabbian, Giulio, Feng, Chang, Ferraro, Simone, Filippini, Jeffrey P, Flauger, Raphael, Flaugher, Brenna, Fraisse, Aurelien A, Frolov, Andrei, Galitzki, Nicholas, Gallardo, Patricio A, Galli, Silvia, Ganga, Ken, Gerbino, Martina, Gluscevic, Vera, Goeckner-Wald, Neil, Green, Daniel, Grin, Daniel, Grohs, Evan, Gualtieri, Riccardo, Gudmundsson, Jon E, Gullett, Ian, Gupta, Nikhel, Habib, Salman, Halpern, Mark, Halverson, Nils W, Hanany, Shaul, Harrington, Kathleen, Hasegawa, Masaya, and Hasselfield, Matthew

Subjects
astro-ph.CO
Abstract

CMB-S4---the next-generation ground-based cosmic microwave background (CMB)experiment---is set to significantly advance the sensitivity of CMBmeasurements and enhance our understanding of the origin and evolution of theUniverse, from the highest energies at the dawn of time through the growth ofstructure to the present day. Among the science cases pursued with CMB-S4, thequest for detecting primordial gravitational waves is a central driver of theexperimental design. This work details the development of a forecastingframework that includes a power-spectrum-based semi-analytic projection tool,targeted explicitly towards optimizing constraints on the tensor-to-scalarratio, $r$, in the presence of Galactic foregrounds and gravitational lensingof the CMB. This framework is unique in its direct use of information from theachieved performance of current Stage 2--3 CMB experiments to robustly forecastthe science reach of upcoming CMB-polarization endeavors. The methodologyallows for rapid iteration over experimental configurations and offers aflexible way to optimize the design of future experiments given a desiredscientific goal. To form a closed-loop process, we couple this semi-analytictool with map-based validation studies, which allow for the injection ofadditional complexity and verification of our forecasts with severalindependent analysis methods. We document multiple rounds of forecasts forCMB-S4 using this process and the resulting establishment of the currentreference design of the primordial gravitational-wave component of the Stage-4experiment, optimized to achieve our science goals of detecting primordialgravitational waves for $r > 0.003$ at greater than $5\sigma$, or, in theabsence of a detection, of reaching an upper limit of $r < 0.001$ at $95\%$ CL.

Published
2020

17. Primordial Non-Gaussianity

Author

Meerburg, P Daniel, Green, Daniel, Abidi, Muntazir, Amin, Mustafa A, Adshead, Peter, Ahmed, Zeeshan, Alonso, David, Ansarinejad, Behzad, Armstrong, Robert, Avila, Santiago, Baccigalupi, Carlo, Baldauf, Tobias, Ballardini, Mario, Bandura, Kevin, Bartolo, Nicola, Battaglia, Nicholas, Baumann, Daniel, Bavdhankar, Chetan, Bernal, José Luis, Beutler, Florian, Biagetti, Matteo, Bischoff, Colin, Blazek, Jonathan, Bond, J Richard, Borrill, Julian, Bouchet, François R, Bull, Philip, Burgess, Cliff, Byrnes, Christian, Calabrese, Erminia, Carlstrom, John E, Castorina, Emanuele, Challinor, Anthony, Chang, Tzu-Ching, Chaves-Montero, Jonas, Chen, Xingang, Yeche, Christophe, Cooray, Asantha, Coulton, William, Crawford, Thomas, Chisari, Elisa, Cyr-Racine, Francis-Yan, D'Amico, Guido, de Bernardis, Paolo, de la Macorra, Axel, Doré, Olivier, Duivenvoorden, Adri, Dunkley, Joanna, Dvorkin, Cora, Eggemeier, Alexander, Escoffier, Stephanie, Essinger-Hileman, Tom, Fasiello, Matteo, Ferraro, Simone, Flauger, Raphael, Font-Ribera, Andreu, Foreman, Simon, Friedrich, Oliver, Garcia-Bellido, Juan, Gerbino, Martina, Gluscevic, Vera, Goon, Garrett, Gorski, Krzysztof M, Gudmundsson, Jon E, Gupta, Nikhel, Hanany, Shaul, Handley, Will, Hawken, Adam J, Hill, J Colin, Hirata, Christopher M, Hložek, Renée, Holder, Gilbert, Huterer, Dragan, Kamionkowski, Marc, Karkare, Kirit S, Keeley, Ryan E, Kinney, William, Kisner, Theodore, Kneib, Jean-Paul, Knox, Lloyd, Koushiappas, Savvas M, Kovetz, Ely D, Koyama, Kazuya, L'Huillier, Benjamin, Lahav, Ofer, Lattanzi, Massimiliano, Lee, Hayden, Liguori, Michele, Loverde, Marilena, Madhavacheril, Mathew, Maldacena, Juan, Marsh, MC David, Masui, Kiyoshi, Matarrese, Sabino, McAllister, Liam, McMahon, Jeff, McQuinn, Matthew, Meyers, Joel, Mirbabayi, Mehrdad, and Dizgah, Azadeh Moradinezhad

Subjects
astro-ph.CO, hep-th
Abstract

Our current understanding of the Universe is established through the pristinemeasurements of structure in the cosmic microwave background (CMB) and thedistribution and shapes of galaxies tracing the large scale structure (LSS) ofthe Universe. One key ingredient that underlies cosmological observables isthat the field that sources the observed structure is assumed to be initiallyGaussian with high precision. Nevertheless, a minimal deviation fromGaussianityis perhaps the most robust theoretical prediction of models thatexplain the observed Universe; itis necessarily present even in the simplestscenarios. In addition, most inflationary models produce far higher levels ofnon-Gaussianity. Since non-Gaussianity directly probes the dynamics in theearly Universe, a detection would present a monumental discovery in cosmology,providing clues about physics at energy scales as high as the GUT scale.

Published
2019

18. SZE Observables, Pressure Profiles and Center Offsets in Magneticum Simulation Galaxy Clusters

Author

Gupta, Nikhel, Saro, Alex, Mohr, Joe, Dolag, Klaus., and Liu, Jiayi

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a detailed study of the galaxy cluster thermal \ac{sze} signal $Y$ and pressure profiles using {\it Magneticum} Pathfinder hydrodynamical simulations. With a sample of 50,000 galaxy clusters ($M_{\rm 500c}>1.4\times10^{14} \rm M_{\odot}$) out to $z=2$, we find significant variations in the shape of the pressure profile with mass and redshift and present a new generalized NFW model that follows these trends. We show that the thermal pressure at $R_{\rm 500c}$ accounts for only 80~percent of the pressure required to maintain hydrostatic equilibrium, and therefore even idealized hydrostatic mass estimates would be biased at the 20~percent level. We compare the cluster \ac{sze} signal extracted from a sphere with different virial-like radii, a virial cylinder within a narrow redshift slice and the full light cone, confirming small scatter ($\sigma_{\ln Y}\simeq 0.087$) in the sphere and showing that structure immediately surrounding clusters increases the scatter and strengthens non self-similar redshift evolution in the cylinder. Uncorrelated large scale structure along the line of sight leads to an increase in the \ac{sze} signal and scatter that is more pronounced for low mass clusters, resulting in non self-similar trends in both mass and redshift and a mass dependent scatter that is $\sim0.16$ at low masses. The scatter distribution is consistent with log-normal in all cases. We present a model of the offsets between the center of the gravitational potential and the \ac{sze} center that follows the variations with cluster mass and redshift., Comment: 20 pages, 15 figures, submitted to MNRAS

Published
2016
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19. ASKAP reveals the radio tail structure of the Corkscrew Galaxy shaped by its passage through the Abell 3627 cluster.

Author

Koribalski, Bärbel S, Duchesne, Stefan W, Lenc, Emil, Venturi, Tiziana, Botteon, Andrea, Shabala, Stanislav S, Vernstrom, Tessa, Carretti, Ettore, Norris, Ray P, Anderson, Craig, Hopkins, Andrew M, Riseley, C J, Gupta, Nikhel, and Velović, Velibor

Subjects
GALAXY clusters, SHOCK waves, PHASED array antennas, RADIO interferometers, SHEARING force, RADIO galaxies
Abstract

Among the bent-tail radio galaxies common in galaxy clusters are some with long, collimated tails (so-called head-tail galaxies) shaped by their interactions with the intracluster medium (ICM). Here, we report the discovery of intricate filamentary structure in and beyond the ∼28 arcmin (570 kpc) long, helical radio tail of the Corkscrew Galaxy (1610–60.5, ESO 137-G007), which resides in the X-ray bright cluster Abell 3627 (D = 70 Mpc). Deep radio continuum data were obtained with wide-field phased array feeds on the Australian Square Kilometer Array Pathfinder (ASKAP) at 944 MHz and 1.4 GHz. While the bright (young) part of the Corkscrew Galaxy tail is highly collimated, the faint (old) part shows increasing oscillation amplitudes, break-ups, and filaments. We find a stunning set of arc-shaped radio filaments beyond and mostly orthogonal to the collimated Corkscrew tail end, forming a partial bubble. This may be the first detection of a 'proto-lobe' previously seen in 3D MHD simulations, formed by the face-on impact of the Corkscrew Galaxy with a shock front in the cluster outskirts. Interactions of the radio galaxy tail with the ICM are likely responsible for the tail collimation and shear forces within the ICM for its increasingly filamentary structure. We also report the discovery of small (∼20–30 kpc) ram-pressure stripped radio tails in four Abell 3627 cluster galaxies, located between the Corkscrew Galaxy and its prominent neighbour, the wide-angle tail (WAT) radio galaxy 1610–60.8 (ESO 137-G006). [ABSTRACT FROM AUTHOR]

Published
2024
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20. The Physalis system: discovery of ORC-like radio shells around a massive pair of interacting early-type galaxies with offset X-ray emission.

Author

Koribalski, Bärbel S, Khabibullin, Ildar, Dolag, Klaus, Churazov, Eugene, Norris, Ray P, Carretti, Ettore, Hopkins, Andrew M, Vernstrom, Tessa, Shabala, Stanislav S, and Gupta, Nikhel

Subjects
GALAXY clusters, RADIO galaxies, GALACTIC evolution, ACTIVE galactic nuclei, GALAXY formation
Abstract

We present the discovery of large radio shells around a massive pair of interacting galaxies and extended diffuse X-ray emission within the shells. The radio data were obtained with the Australian Square Kilometre Array Pathfinder (ASKAP) in two frequency bands centred at 944 MHz and 1.4 GHz, respectively, while the X-ray data are from the XMM–Newton observatory. The host galaxy pair, which consists of the early-type galaxies ESO 184-G042 and LEDA 418116, is part of a loose group at a distance of only 75 Mpc (redshift |$z = 0.017$|⁠). The observed outer radio shells (diameter |${\sim}$| 145 kpc) and ridge-like central emission of the system, ASKAP J1914−5433 (Physalis), are likely associated with merger shocks during the formation of the central galaxy (ESO 184-G042) and resemble the new class of odd radio circles (ORCs). This is supported by the brightest X-ray emission found offset from the centre of the Physalis system, instead centred at the less massive galaxy, LEDA 418116. The host galaxy pair is embedded in an irregular envelope of diffuse light, highlighting ongoing interactions. We complement our combined radio and X-ray study with high-resolution simulations of the circumgalactic medium (CGM) around galaxy mergers from the Magneticum project to analyse the evolutionary state of the Physalis system. We argue that ORCs/radio shells could be produced by a combination of energy release from the central active galactic nucleus and subsequent lightening up in radio emission by merger shocks travelling through the CGM of these systems. [ABSTRACT FROM AUTHOR]

Published
2024
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21. RG-CAT: Detection Pipeline and Catalogue of Radio Galaxies in the EMU Pilot Survey

Author

Gupta, Nikhel, primary, Norris, Ray P., additional, Hayder, Zeeshan, additional, Huynh, Minh, additional, Petersson, Lars, additional, Wang, X. Rosalind, additional, Hopkins, Andrew M., additional, Andernach, Heinz, additional, Gordon, Yjan, additional, Riggi, Simone, additional, Yew, Miranda, additional, Crawford, Evan J., additional, Koribalski, Bärbel, additional, Filipović, Miroslav D., additional, Kapińska, Anna D., additional, Shabala, Stanislav, additional, Vernstrom, Tessa, additional, and Marvil, Joshua R., additional

Published
2024
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23. CMB-S4

Author

Collaboration, The CMB-S4, Abazajian, Kevork, Addison, Graeme E., Adshead, Peter, Ahmed, Zeeshan, Akerib, Daniel, Ali, Aamir, Allen, Steven W., Alonso, David, Alvarez, Marcelo, Amin, Mustafa A., Anderson, Adam, Arnold, Kam S., Ashton, Peter, Baccigalupi, Carlo, Bard, Debbie, Barkats, Denis, Barron, Darcy, Barry, Peter S., Bartlett, James G., Thakur, Ritoban Basu, Battaglia, Nicholas, Bean, Rachel, Bebek, Chris, Bender, Amy N., Benson, Bradford A., Bianchini, Federico, Bischoff, Colin A., Bleem, Lindsey, Bock, James J., Bocquet, Sebastian, Boddy, Kimberly K., Bond, J. Richard, Borrill, Julian, Bouchet, François R., Brinckmann, Thejs, Brown, Michael L., Bryan, Sean, Buza, Victor, Byrum, Karen, Caimapo, Carlos Hervias, Calabrese, Erminia, Calafut, Victoria, Caldwell, Robert, Carlstrom, John E., Carron, Julien, Cecil, Thomas, Challinor, Anthony, Chang, Clarence L., Chinone, Yuji, Cho, Hsiao-Mei Sherry, Cooray, Asantha, Coulton, Will, Crawford, Thomas M., Crites, Abigail, Cukierman, Ari, Cyr-Racine, Francis-Yan, de Haan, Tijmen, Delabrouille, Jacques, Devlin, Mark, Di Valentino, Eleonora, Dierickx, Marion, Dobbs, Matt, Duff, Shannon, Dunkley, Jo, Dvorkin, Cora, Eimer, Joseph, Elleflot, Tucker, Errard, Josquin, Essinger-Hileman, Thomas, Fabbian, Giulio, Feng, Chang, Ferraro, Simone, Filippini, Jeffrey P., Flauger, Raphael, Flaugher, Brenna, Fraisse, Aurelien A., Frolov, Andrei, Galitzki, Nicholas, Gallardo, Patricio A., Galli, Silvia, Ganga, Ken, Gerbino, Martina, Gluscevic, Vera, Goeckner-Wald, Neil, Green, Daniel, Grin, Daniel, Grohs, Evan, Gualtieri, Riccardo, Gudmundsson, Jon E., Gullett, Ian, Gupta, Nikhel, Habib, Salman, Halpern, Mark, Halverson, Nils W., Hanany, Shaul, Harrington, Kathleen, Hasegawa, Masaya, Hasselfield, Matthew, Hazumi, Masashi, Heitmann, Katrin, Henderson, Shawn, Hensley, Brandon, Hill, Charles, Hill, J. Colin, Hlozek, Renée, Ho, Shuay-Pwu Patty, Hoang, Thuong, Holder, Gil, Holzapfel, William, Hood, John, Hubmayr, Johannes, Huffenberger, Kevin M., Hui, Howard, Irwin, Kent, Jeong, Oliver, Johnson, Bradley R., Jones, William C., Kang, Jae Hwan, Karkare, Kirit S., Katayama, Nobuhiko, Keskitalo, Reijo, Kisner, Theodore, Knox, Lloyd, Koopman, Brian J., Kosowsky, Arthur, Kovac, John, Kovetz, Ely D., Kuhlmann, Steve, Kuo, Chao-lin, Kusaka, Akito, Lähteenmäki, Anne, Lawrence, Charles R., Lee, Adrian T., Lewis, Antony, Li, Dale, Linder, Eric, Loverde, Marilena, Lowitz, Amy, Lubin, Phil, Madhavacheril, Mathew S., Mantz, Adam, Marques, Gabriela, Matsuda, Frederick, Mauskopf, Philip, McCarrick, Heather, McMahon, Jeffrey, Meerburg, P. Daniel, Melin, Jean-Baptiste, Menanteau, Felipe, Meyers, Joel, Millea, Marius, Mohr, Joseph, Moncelsi, Lorenzo, Monzani, Maria, Mroczkowski, Tony, Mukherjee, Suvodip, Nagy, Johanna, Namikawa, Toshiya, Nati, Federico, Natoli, Tyler, Newburgh, Laura, Niemack, Michael D., Nishino, Haruki, Nord, Brian, Novosad, Valentine, O'Brient, Roger, Padin, Stephen, Palladino, Steven, Partridge, Bruce, Petravick, Don, Pierpaoli, Elena, Pogosian, Levon, Prabhu, Karthik, Pryke, Clement, Puglisi, Giuseppe, Racine, Benjamin, Rahlin, Alexandra, Rao, Mayuri Sathyanarayana, Raveri, Marco, Reichardt, Christian L., Remazeilles, Mathieu, Rocha, Graca, Roe, Natalie A., Roy, Anirban, Ruhl, John E., Salatino, Maria, Saliwanchik, Benjamin, Schaan, Emmanuel, Schillaci, Alessandro, Schmitt, Benjamin, Schmittfull, Marcel M., Scott, Douglas, Sehgal, Neelima, Shandera, Sarah, Sherwin, Blake D., Shirokoff, Erik, Simon, Sara M., Slosar, Anze, Spergel, David, Germaine, Tyler St., Staggs, Suzanne T., Stark, Antony, Starkman, Glenn D., Stompor, Radek, Stoughton, Chris, Suzuki, Aritoki, Tajima, Osamu, Teply, Grant P., Thompson, Keith, Thorne, Ben, Timbie, Peter, Tomasi, Maurizio, Tristram, Matthieu, Tucker, Gregory, Umiltà, Caterina, van Engelen, Alexander, Vavagiakis, Eve M., Vieira, Joaquin D., Vieregg, Abigail G., Wagoner, Kasey, Wallisch, Benjamin, Wang, Gensheng, Watson, Scott, Westbrook, Ben, Whitehorn, Nathan, Wollack, Edward J., Wu, W. L. Kimmy, Xu, Zhilei, Yang, H. Y. Eric, Yasini, Siavash, Yefremenko, Volodymyr G., Yoon, Ki Won, Young, Edward, Yu, Cyndia, Zonca, Andrea, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Théorique - UMR CNRS 3681 (IPHT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), CMB-S4, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Paris-Sud - Paris 11 (UP11), Apollo - University of Cambridge Repository, Van Swinderen Institute for Particle Physics and G, Cosmic Frontier, Abazajian, K, Addison, G, Adshead, P, Ahmed, Z, Akerib, D, Ali, A, Allen, S, Alonso, D, Alvarez, M, Amin, M, Anderson, A, Arnold, K, Ashton, P, Baccigalupi, C, Bard, D, Barkats, D, Barron, D, Barry, P, Bartlett, J, Basu Thakur, R, Battaglia, N, Bean, R, Bebek, C, Bender, A, Benson, B, Bianchini, F, Bischoff, C, Bleem, L, Bock, J, Bocquet, S, Boddy, K, Richard Bond, J, Borrill, J, Bouchet, F, Brinckmann, T, Brown, M, Bryan, S, Buza, V, Byrum, K, Hervias Caimapo, C, Calabrese, E, Calafut, V, Caldwell, R, Carlstrom, J, Carron, J, Cecil, T, Challinor, A, Chang, C, Chinone, Y, Sherry Cho, H, Cooray, A, Coulton, W, Crawford, T, Crites, A, Cukierman, A, Cyr-Racine, F, De Haan, T, Delabrouille, J, Devlin, M, Di Valentino, E, Dierickx, M, Dobbs, M, Duff, S, Dvorkin, C, Eimer, J, Elleflot, T, Errard, J, Essinger-Hileman, T, Fabbian, G, Feng, C, Ferraro, S, Filippini, J, Flauger, R, Flaugher, B, Fraisse, A, Frolov, A, Galitzki, N, Gallardo, P, Galli, S, Ganga, K, Gerbino, M, Gluscevic, V, Goeckner-Wald, N, Green, D, Grin, D, Grohs, E, Gualtieri, R, Gudmundsson, J, Gullett, I, Gupta, N, Habib, S, Halpern, M, Halverson, N, Hanany, S, Harrington, K, Hasegawa, M, Hasselfield, M, Hazumi, M, Heitmann, K, Henderson, S, Hensley, B, Hill, C, Colin Hill, J, Hlozek, R, Patty Ho, S, Hoang, T, Holder, G, Holzapfel, W, Hood, J, Hubmayr, J, Huffenberger, K, Hui, H, Irwin, K, Jeong, O, Johnson, B, Jones, W, Hwan Kang, J, Karkare, K, Katayama, N, Keskitalo, R, Kisner, T, Knox, L, Koopman, B, Kosowsky, A, Kovac, J, Kovetz, E, Kuhlmann, S, Kuo, C, Kusaka, A, Lahteenmaki, A, Lawrence, C, Lee, A, Lewis, A, Li, D, Linder, E, Loverde, M, Lowitz, A, Lubin, P, Madhavacheril, M, Mantz, A, Marques, G, Matsuda, F, Mauskopf, P, Mccarrick, H, Mcmahon, J, Daniel Meerburg, P, Melin, J, Menanteau, F, Meyers, J, Millea, M, Mohr, J, Moncelsi, L, Monzani, M, Mroczkowski, T, Mukherjee, S, Nagy, J, Namikawa, T, Nati, F, Natoli, T, Newburgh, L, Niemack, M, Nishino, H, Nord, B, Novosad, V, O'Brient, R, Padin, S, Palladino, S, Partridge, B, Petravick, D, Pierpaoli, E, Pogosian, L, Prabhu, K, Pryke, C, Puglisi, G, Racine, B, Rahlin, A, Sathyanarayana Rao, M, Raveri, M, Reichardt, C, Remazeilles, M, Rocha, G, Roe, N, Roy, A, Ruhl, J, Salatino, M, Saliwanchik, B, Schaan, E, Schillaci, A, Schmitt, B, Schmittfull, M, Scott, D, Sehgal, N, Shandera, S, Sherwin, B, Shirokoff, E, Simon, S, Slosar, A, Spergel, D, S, T, Staggs, S, Stark, A, Starkman, G, Stompor, R, Stoughton, C, Suzuki, A, Tajima, O, Teply, G, Thompson, K, Thorne, B, Timbie, P, Tomasi, M, Tristram, M, Tucker, G, Umilta, C, Van Engelen, A, Vavagiakis, E, Vieira, J, Vieregg, A, Wagoner, K, Wallisch, B, Wang, G, Watson, S, Westbrook, B, Whitehorn, N, Wollack, E, Kimmy Wu, W, Xu, Z, Eric Yang, H, Yasini, S, Yefremenko, V, Won Yoon, K, Young, E, Yu, C, Zonca, A, University of California Irvine, Johns Hopkins University, University of Illinois at Urbana-Champaign, SLAC National Accelerator Laboratory, University of California Berkeley, Stanford University, University of Oxford, Rice University, Fermi National Accelerator Laboratory, University of California San Diego, International School for Advanced Studies, Lawrence Berkeley National Laboratory, Harvard University, University of New Mexico, Argonne National Laboratory, Université Paris-Diderot, California Institute of Technology, Cornell University, University of Melbourne, University of Cincinnati, Ludwig Maximilian University of Munich, University of Toronto, UMR7095, Stony Brook University, University of Manchester, Arizona State University, Florida State University, Cardiff University, Dartmouth College, University of Geneva, University of Cambridge, The University of Tokyo, University of Groningen, University of Chicago, University of Pennsylvania, McGill University, National Institute of Standards and Technology, NASA Goddard Space Flight Center, University of Sussex, Princeton University, Simon Fraser University, National Institute for Nuclear Physics, Haverford College, Stockholm University, Case Western Reserve University, University of British Columbia, University of Colorado Boulder, University of Minnesota Twin Cities, University of Michigan, Ann Arbor, Simons Foundation, Columbia University, University of Virginia, University of California Davis, Yale University, University of Pittsburgh, Ben-Gurion University of the Negev, Department of Electronics and Nanoengineering, Jet Propulsion Laboratory, University of California Santa Barbara, Perimeter Institute for Theoretical Physics, Service d'Astrophysique CEA, European Southern Observatory, Washington University St. Louis, University of Milan - Bicocca, University of Southern California, Institute for Advanced Studies, Pennsylvania State University, Brookhaven National Laboratory, Kyoto University, University of Wisconsin-Madison, University of Milano, Université Paris-Saclay, Brown University, Syracuse University, University of California Los Angeles, Aalto-yliopisto, and Aalto University

Subjects
Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmology, CMB, Settore FIS/05, Space and Planetary Science, astro-ph.CO, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Galaxies and Cosmology, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

CMB-S4---the next-generation ground-based cosmic microwave background (CMB) experiment---is set to significantly advance the sensitivity of CMB measurements and enhance our understanding of the origin and evolution of the Universe, from the highest energies at the dawn of time through the growth of structure to the present day. Among the science cases pursued with CMB-S4, the quest for detecting primordial gravitational waves is a central driver of the experimental design. This work details the development of a forecasting framework that includes a power-spectrum-based semi-analytic projection tool, targeted explicitly towards optimizing constraints on the tensor-to-scalar ratio, $r$, in the presence of Galactic foregrounds and gravitational lensing of the CMB. This framework is unique in its direct use of information from the achieved performance of current Stage 2--3 CMB experiments to robustly forecast the science reach of upcoming CMB-polarization endeavors. The methodology allows for rapid iteration over experimental configurations and offers a flexible way to optimize the design of future experiments given a desired scientific goal. To form a closed-loop process, we couple this semi-analytic tool with map-based validation studies, which allow for the injection of additional complexity and verification of our forecasts with several independent analysis methods. We document multiple rounds of forecasts for CMB-S4 using this process and the resulting establishment of the current reference design of the primordial gravitational-wave component of the Stage-4 experiment, optimized to achieve our science goals of detecting primordial gravitational waves for $r > 0.003$ at greater than $5��$, or, in the absence of a detection, of reaching an upper limit of $r < 0.001$ at $95\%$ CL., 24 pages, 8 figures, 9 tables, submitted to ApJ. arXiv admin note: text overlap with arXiv:1907.04473

Published
2022
Full Text
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24. The Massive and Distant Clusters of WISE Survey. VI. Stellar Mass Fractions of a Sample of High-redshift Infrared-selected Clusters

Author

MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Physics, Decker, Bandon, Brodwin, Mark, Abdulla, Zubair, Gonzalez, Anthony H, Marrone, Daniel P, O’Donnell, Christine, Stanford, SA, Wylezalek, Dominika, Carlstrom, John E, Eisenhardt, Peter RM, Mantz, Adam, Mo, Wenli, Moravec, Emily, Stern, Daniel, Aldering, Greg, Ashby, Matthew LN, Boone, Kyle, Hayden, Brian, Gupta, Nikhel, McDonald, Michael A., MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Physics, Decker, Bandon, Brodwin, Mark, Abdulla, Zubair, Gonzalez, Anthony H, Marrone, Daniel P, O’Donnell, Christine, Stanford, SA, Wylezalek, Dominika, Carlstrom, John E, Eisenhardt, Peter RM, Mantz, Adam, Mo, Wenli, Moravec, Emily, Stern, Daniel, Aldering, Greg, Ashby, Matthew LN, Boone, Kyle, Hayden, Brian, Gupta, Nikhel, and McDonald, Michael A.

Abstract

© 2019. The American Astronomical Society. All rights reserved. We present measurements of the stellar mass fractions ( f∗) for a sample of high-redshift (0.93≤.z≤1.32) infrared-selected galaxy clusters from the Massive and Distant Clusters of WISE Survey (MaDCoWS) and compare them to the stellar mass fractions of Sunyaev-Zel-dovich (SZ) effect-selected clusters in a similar mass and redshift range from the South Pole Telescope (SPT)-SZ Survey. We do not find a significant difference in mean f∗ between the two selection methods; though, we do find an unexpectedly large range in f∗ for the SZ-selected clusters. In addition, we measure the luminosity function of the MaDCoWS clusters and find m∗ = 19.41 ± 0.07, similar to other studies of clusters at or near our redshift range. Finally, we present SZ detections and masses for seven MaDCoWS clusters and new spectroscopic redshifts for five MaDCoWS clusters. One of these new clusters, MOO J1521+0452 at z = 1.31, is the most distant MaDCoWS cluster confirmed to date.

Published
2022

25. Performance and characterization of the SPT-3G digital frequency-domain multiplexed readout system using an improved noise and crosstalk model

Author

Montgomery, Joshua, primary, Ade, Peter A. R., additional, Ahmed, Zeeshan, additional, Anderes, Ethan, additional, Anderson, Adam J., additional, Archipley, Melanie, additional, Avva, Jessica S., additional, Aylor, Kevin, additional, Balkenhol, Lennart, additional, Barry, Peter S., additional, Thakur, Ritoban B., additional, Benabed, Karim, additional, Bender, Amy N., additional, Benson, Bradford A., additional, Bianchini, Federico, additional, Bleem, Lindsey E., additional, Bouchet, Francois R., additional, Bryant, Lincoln, additional, Byrum, Karen, additional, Carlstrom, John E., additional, Carter, Faustin W., additional, Cecil, Thomas W., additional, Chang, Clarence L., additional, Chaubal, Prakrut, additional, Chen, Geoffrey, additional, Cho, Hsiaomei, additional, Chou, Ti-Lin, additional, Cliche, Jean-Francois, additional, Crawford, Tom M., additional, Cukierman, Ari, additional, Daley, Cail, additional, de Haan, Tijmen, additional, Denison, Edward V., additional, Dibert, Karia, additional, Ding, Junjia, additional, Dobbs, Matt A., additional, Dutcher, Daniel, additional, Elleflot, Tucker, additional, Everett, Wendeline, additional, Feng, Cahng, additional, Ferguson, Kyle R., additional, Foster, Allen, additional, Fu, Jianyang, additional, Galli, Silvia, additional, Gambrel, Anne E., additional, Gardner, Robert W., additional, Goeckner-Wald, Neil, additional, Groh, John C., additional, Gualtieri, Riccardo, additional, Guns, Sam, additional, Gupta, Nikhel, additional, Guyser, Robert, additional, Halverson, Nils W., additional, Harke-Hosemann, Angelina H., additional, Harrington, Nicholas L., additional, Henning, Jason W., additional, Hilton, Gene C., additional, Hivon, Eric, additional, Holzapfel, William L., additional, Hood, John C., additional, Howe, Doug, additional, Huang, Nicholas, additional, Irwin, Kent D., additional, Jeong, Oliver B., additional, Jonas, Michelle, additional, Jones, Adam, additional, Khaire, Trupti S., additional, Knox, Lloyd, additional, Kofman, Anna M., additional, Korman, Milo, additional, Kubik, Donna L., additional, Kuhlmann, Stephen, additional, Kuo, Chao-Lin, additional, Lee, Adrian T., additional, Leitch, Erik M., additional, Lowitz, Amy E., additional, Lu, Chunyu, additional, Meyer, Stephan S., additional, Michalik, Daniel, additional, Millea, Marius, additional, Nadolski, Andrew, additional, Natoli, Tyler, additional, Nguyen, Hogan, additional, Noble, Gavin I., additional, Novosad, Valentine, additional, Omori, Yuuki, additional, Padin, Steve, additional, Pan, Zhaodi, additional, Paschos, Pascal, additional, Pearson, John, additional, Posada, Chrystian M., additional, Prabhu, Karthik, additional, Quan, Wei, additional, Rahlin, Alexandra, additional, Reichardt, Christian L., additional, Riebel, David, additional, Riedel, Benedikt, additional, Rouble, Maclean, additional, Ruhl, John E., additional, Sayre, James T., additional, Schiappucci, Eduardo, additional, Shirokoff, Erik, additional, Smecher, Graeme, additional, Sobrin, Joshua A., additional, Stark, Antony A., additional, Stephen, Judith, additional, Story, Kyle T., additional, Suzuki, Aritoki, additional, Thompson, Keith L., additional, Thorne, Ben, additional, Tucker, Carole, additional, Umilta, Caterina, additional, Vale, Leila R., additional, Vanderlinde, Keith, additional, Vieira, Joaquin D., additional, Wang, Gensheng, additional, Whitehorn, Nathan, additional, Wu, Wai L. K., additional, Yefremenko, Volodymyr, additional, Yoon, Ki W., additional, and Young, Matt R., additional

Published
2022
Full Text
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27. The Massive and Distant Clusters of WISE Survey. VI. Stellar Mass Fractions of a Sample of High-redshift Infrared-selected Clusters

Author

Decker, Bandon, Brodwin, Mark, Abdulla, Zubair, Gonzalez, Anthony H, Marrone, Daniel P, O’Donnell, Christine, Stanford, SA, Wylezalek, Dominika, Carlstrom, John E, Eisenhardt, Peter RM, Mantz, Adam, Mo, Wenli, Moravec, Emily, Stern, Daniel, Aldering, Greg, Ashby, Matthew LN, Boone, Kyle, Hayden, Brian, Gupta, Nikhel, McDonald, Michael A, Decker, Bandon, Brodwin, Mark, Abdulla, Zubair, Gonzalez, Anthony H, Marrone, Daniel P, O’Donnell, Christine, Stanford, SA, Wylezalek, Dominika, Carlstrom, John E, Eisenhardt, Peter RM, Mantz, Adam, Mo, Wenli, Moravec, Emily, Stern, Daniel, Aldering, Greg, Ashby, Matthew LN, Boone, Kyle, Hayden, Brian, Gupta, Nikhel, and McDonald, Michael A

Abstract

© 2019. The American Astronomical Society. All rights reserved. We present measurements of the stellar mass fractions ( f∗) for a sample of high-redshift (0.93≤.z≤1.32) infrared-selected galaxy clusters from the Massive and Distant Clusters of WISE Survey (MaDCoWS) and compare them to the stellar mass fractions of Sunyaev-Zel-dovich (SZ) effect-selected clusters in a similar mass and redshift range from the South Pole Telescope (SPT)-SZ Survey. We do not find a significant difference in mean f∗ between the two selection methods; though, we do find an unexpectedly large range in f∗ for the SZ-selected clusters. In addition, we measure the luminosity function of the MaDCoWS clusters and find m∗ = 19.41 ± 0.07, similar to other studies of clusters at or near our redshift range. Finally, we present SZ detections and masses for seven MaDCoWS clusters and new spectroscopic redshifts for five MaDCoWS clusters. One of these new clusters, MOO J1521+0452 at z = 1.31, is the most distant MaDCoWS cluster confirmed to date.

Published
2021

28. Astro2020 Science White Paper: Primordial Non-Gaussianity

Author

Meerburg, P. Daniel, Green, Daniel, Abidi, Muntazir, Amin, Mustafa A., Adshead, Peter, Ahmed, Zeeshan, Alonso, David, Ansarinejad, Behzad, Armstrong, Robert, Ávila, Santiago, Baccigalupi, Carlo, Baldauf, Tobias, Ballardini, Mario, Bandura, Kevin, Bartolo, Nicola, Battaglia, Nicholas, Baumann, Daniel, Bavdhankar, Chetan, Bernal, José Luis, Beutler, Florian, Biagetti, Matteo, Bischoff, Colin, Blazek, Jonathan, Bond, J. Richard, Borrill, Julian, Bouchet, François R., Bull, Philip, Burgess, Cliff, Byrnes, Christian, Calabrese, Erminia, Carlstrom, John E., Castorina, Emanuele, Challinor, Anthony, Chang, Tzu-Ching, Chaves-Montero, Jonas, Chen, Xingang, Yeche, Christophe, Cooray, Asantha, Coulton, William, Crawford, Thomas, Chisari, Elisa, Cyr-Racine, Francis-Yan, d'Amico, Guido, de Bernardis, Paolo, de La Macorra, Axel, Dore, Olivier, Duivenvoorden, Adri, Dunkley, Joanna, Dvorkin, Cora, Eggemeier, Alexander, Escoffier, Stephanie, Essinger-Hileman, Tom, Fasiello, Matteo, Ferraro, Simone, Flauger, Raphael, Font-Ribera, Andreu, Foreman, Simon, Friedrich, Oliver, Garcia-Bellido, Juan, Gerbino, Martina, Gluscevic, Vera, Goon, Garrett, Gorski, Krzysztof M., Gudmundsson, Jon E., Gupta, Nikhel, Hanany, Shaul, Handley, Will, Hawken, Adam J., Hill, J. Colin, Hirata, Christopher M., Hložek, Renée, Holder, Gilbert, Huterer, Dragan, Kamionkowski, Marc, Karkare, Kirit S., Keeley, Ryan E., Kinney, William, Kisner, Theodore, Kneib, Jean-Paul, Knox, Lloyd, Koushiappas, Savvas M., Kovetz, Ely D., Koyama, Kazuya, L'Huillier, Benjamin, Lahav, Ofer, Lattanzi, Massimiliano, Lee, Hayden, Liguori, Michele, Loverde, Marilena, Madhavacheril, Mathew, Maldacena, Juan, Marsh, M. C. David, Masui, Kiyoshi, Matarrese, Sabino, Mcallister, Liam, Mcmahon, Jeff, Mcquinn, Matthew, Meyers, Joel, Mirbabayi, Mehrdad, Dizgah, Azadeh Moradinezhad, Motloch, Pavel, Mukherjee, Suvodip, Muñoz, Julian B., Myers, Adam D., Nagy, Johanna, Naselsky, Pavel, Nati, Federico, Nicolis, Alberto, Niemack, Michael D., Niz, Gustavo, Nomerotski, Andrei, Page, Lyman, Pajer, Enrico, Padmanabhan, Hamsa, Palma, Gonzalo A., Peiris, Hiranya V., Percival, Will J., Piacentni, Francesco, Pimentel, Guilherme L., Pogosian, Levon, Prescod-Weinstein, Chanda, Pryke, Clement, Puglisi, Giuseppe, Racine, Benjamin, Stompor, Radek, Raveri, Marco, Remazeilles, Mathieu, Rocha, Gracca, Ross, Ashley J., Rossi, Graziano, Ruhl, John, Sasaki, Misao, Schaan, Emmanuel, Schillaci, Alessandro, Schmittfull, Marcel, Sehgal, Neelima, Senatore, Leonardo, Seo, Hee-Jong, Shan, Huanyuan, Shandera, Sarah, Sherwin, Blake D., Silverstein, Eva, Simon, Sara, Slosar, Anže, Staggs, Suzanne, Starkman, Glenn, Stebbins, Albert, Suzuki, Aritoki, Switzer, Eric R., Timbie, Peter, Tolley, Andrew J., Tomasi, Maurizio, Tristram, Matthieu, Trodden, Mark, Tsai, Yu-Dai, Uhlemann, Cora, Umiltà, Caterina, van Engelen, Alexander, Vargas-Magaña, M., Vieregg, Abigail, Wallisch, Benjamin, Wands, David, Wandelt, Benjamin, Wang, Yi, Watson, Scott, Wise, Mark, Wu, W. L. K., Xianyu, Zhong-Zhi, Xu, Weishuang, Yasini, Siavash, Young, Sam, Yutong, Duan, Zaldarriaga, Matias, Zemcov, Michael, Zhao, Gong-Bo, Zheng, Yi, Zhu, Ningfeng, University of Cambridge [UK] (CAM), University of California [San Diego] (UC San Diego), University of California (UC), Universidad Autónoma de Madrid (UAM), Institute of Cosmology and Gravitation [Portsmouth] (ICG), University of Portsmouth, Ecole Polytechnique Fédérale de Lausanne (EPFL), Canadian Institute for Theoretical Astrophysics (CITA), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Argonne National Laboratory [Lemont] (ANL), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Kavli Institute for Particle Astrophysics and Cosmology (KIPAC), Stanford University, Facultad de Ingeniería [Buenos Aires] (FIUBA), Universidad de Buenos Aires [Buenos Aires] (UBA), Dipartimento di Fisica [Roma La Sapienza], Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), University College of London [London] (UCL), National Oceanography Centre [Southampton] (NOC), University of Southampton, Johns Hopkins University (JHU), Korea Astronomy and Space Science Institute (KASI), ICRA and Physics Department, Columbia University [New York], Dipartimento di Fisica 'G. Galilei', Università degli Studi di Padova = University of Padua (Unipd), Kavli Institute for Cosmological Physics [Chicago] (KICP), University of Chicago, School of Physics and Astronomy [Nottingham], University of Nottingham, UK (UON), Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), University of Waterloo [Waterloo], University of New Hampshire (UNH), Istituto Nazionale di Geofisica e Vulcanologia - Sezione di Catania (INGV), Istituto Nazionale di Geofisica e Vulcanologia, Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), University of Manchester [Manchester], Brookhaven National Laboratory [Upton, NY] (BNL), UT-Battelle, LLC-Stony Brook University [SUNY] (SBU), State University of New York (SUNY)-State University of New York (SUNY)-U.S. Department of Energy [Washington] (DOE), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre for Theoretical Cosmology, Institute for Advanced Study Princeton, School of physics and astronomy, Rochester Institute of Technology, University of California, Universidad Autonoma de Madrid (UAM), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Universidad Nacional Autónoma de México (UNAM), Okayama University, Universita degli Studi di Padova, Smithsonian Institution-Harvard University [Cambridge], Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), U.S. Department of Energy [Washington] (DOE)-UT-Battelle, LLC-Stony Brook University [SUNY] (SBU), State University of New York (SUNY)-State University of New York (SUNY), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), and Universidad Nacional Autónoma de México - UNAM (MEXICO)

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::Cosmology and Extragalactic Astrophysics
Abstract

5 pages + references; Submitted to the Astro2020 call for science white papers. This version: fixed author list; International audience; Our current understanding of the Universe is established through the pristine measurements of structure in the cosmic microwave background (CMB) and the distribution and shapes of galaxies tracing the large scale structure (LSS) of the Universe. One key ingredient that underlies cosmological observables is that the field that sources the observed structure is assumed to be initially Gaussian with high precision. Nevertheless, a minimal deviation from Gaussianityis perhaps the most robust theoretical prediction of models that explain the observed Universe; itis necessarily present even in the simplest scenarios. In addition, most inflationary models produce far higher levels of non-Gaussianity. Since non-Gaussianity directly probes the dynamics in the early Universe, a detection would present a monumental discovery in cosmology, providing clues about physics at energy scales as high as the GUT scale.

Published
2019

29. Dark Energy and Modified Gravity

Author

Slosar, Anže, Abazajian, Kevork N., Ahmed, Zeeshan, Alonso, David, Amin, Mustafa A., Ansarinejad, Behzad, Armstrong, Robert, Asorey, Jacobo, Avelino, Arturo, Avila, Santiago, Baccigalupi, Carlo, Ballardini, Mario, Bandura, Kevin, Battaglia, Nicholas, Bender, Amy N., Bennett, Charles, Benson, Bradford, Beutler, Florian, Bianchini, F., Bilicki, Maciej, Bischoff, Colin, Biviano, Andrea, Blazek, Jonathan, Bleem, Lindsey, Bolton, Adam S., Bond, J. Richard, Borrill, Julian, Bose, Sownak, Boucaud, Alexandre, Bouchet, Francois R., Buckley-Geer, Elizabeth, Bull, Philip, Cai, Zheng, Carlstrom, John E., Castander, Francisco J., Castorina, Emanuele, Challinor, Anthony, Chang, Tzu-Ching, Chaves-Montero, Jonas, Chisari, Nora Elisa, Clowe, Douglas, Comparat, Johan, Cooray, Asantha, Croft, Rupert A. C., Cyr-Racine, Francis-Yan, D Amico, Guido, Davis, Tamara M., Dawson, Kyle, Demarteau, Marcel, Dey, Arjun, Dore, Olivier, Yutong, Duan, Dunkley, Joanna, Dvorkin, Cora, Eggemeier, Alexander, Eisenstein, Daniel, Ellison, John, Engelen, Alexander, Escoffier, Stephanie, Fabbian, Giulio, Ferraro, Simone, Ferreira, Pedro G., Font-Ribera, Andreu, Foreman, Simon, Fosalba, Pablo, Friedrich, Oliver, Garcıa-Bellido, Juan, Gerbino, Martina, Gill, Mandeep S. S., Gluscevic, Vera, Gontcho A Gontcho, Satya, Gorski, Krzysztof M., Gruen, Daniel, Gudmundsson, Jon E., Gupta, Nikhel, Guy, Julien, Hanany, Shaul, Handley, Will, Hernández-Aguayo, César, Hill, J. Colin, Hirata, Christopher M., Hlozek, Renée, Holder, Gilbert, Huterer, Dragan, Ishak, Mustapha, Jeltema, Tesla, Jha, Saurabh W., Cohen-Tanugi, Johann, Johnson, Bradley, Kamionkowski, Marc, Karkare, Kirit S., E Keeley, Ryan, Khatri, Rishi, Kirkby, David, Kisner, Theodore, Kneib, Jean-Paul, Knox, Lloyd, Koushiappas, Savvas M., Kovetz, Ely D., Koyama, Kazuya, Krause, Elisabeth, Benjamin L'Huillier, Lahav, Ofer, Lattanzi, Massimiliano, Leonard, Danielle, Levi, Michael, Liguori, Michele, Linden, Anja, Loverde, Marilena, Lukic, Zarija, La Macorra, Axel, Madhavacheril, Mathew, Plazas, Andres, Spurio Mancini, Alessio, Manera, Marc, Mantz, Adam, Martini, Paul, Masui, Kiyoshi, Mcmahon, Jeff, Meerburg, P. Daniel, Mertens, James, Meyers, Joel, More, Surhud, Motloch, Pavel, Mukherjee, Suvodip, Muñoz, Julian B., Myers, Adam D., Nagy, Johanna, Palanque-Delabrouille, Nathalie, Newburgh, Laura, Newman, Jeffrey A., Niemack, Michael D., Niz, Gustavo, Nomerotski, Andrei, O Connor, Paul, Page, Lyman, Palmese, Antonella, Penna-Lima, Mariana, Percival, Will J., Piacentni, Francesco, Pieri, Matthew M., Pierpaoli, Elena, Pogosian, Levon, Prakash, Abhishek, Pryke, Clement, Puglisi, Giuseppe, Stompor, Radek, Raveri, Marco, Reichardt, Christian L., Rhodes, Jason, Rodney, Steven, Rose, Benjamin, Ross, Ashley J., Rossi, Graziano, Ruhl, John, Saliwanchik, Benjamin, Samushia, Lado, Sanchez, Javier, Sasaki, Misao, Schaan, Emmanuel, Schlegel, David J., Schmittfull, Marcel, Schubnell, Michael, Scott, Douglas, Sehgal, Neelima, Senatore, Leonardo, Seo, Hee-Jong, Shafieloo, Arman, Shan, Huanyuan, Sherwin, Blake D., Shi, Feng, Simon, Sara, Slosar, Anze, Staggs, Suzanne, Starkman, Glenn, Stebbins, Albert, Suzuki, Aritoki, Switzer, Eric R., Timbie, Peter, Tolley, Andrew J., Tristram, Matthieu, Trodden, Mark, Troxel, M. A., Uhlemann, Cora, Umilta, Caterina, Urenna-Lopez, L. Arturo, Di Valentino, Eleonora, Vargas-Magana, M., Vieregg, Abigail, Walter, Christopher W., Wang, Yi, Watson, Scott, White, Martin, Whitehorn, Nathan, Wu, W. L. K., Xu, Weishuang, Yasini, Siavash, Zaldarriaga, Matias, Zhao, Gong-Bo, Zheng, Yi, Zhu, Hong-Ming, Zhu, Ningfeng, Zuntz, Joe, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), HEP, INSPIRE, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
cosmological model, Hubble constant, Cosmology and Nongalactic Astrophysics (astro-ph.CO), gravitation: model, FOS: Physical sciences, cosmic background radiation, baryon: oscillation: acoustic, gravitation: lens, statistical analysis, supernova, Sunyaev-Zel'dovich effect, astro-ph.CO, galaxy: cluster, expansion: acceleration, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], dark energy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Despite two decades of tremendous experimental and theoretical progress, the riddle of the accelerated expansion of the Universe remains to be solved. On the experimental side, our understanding of the possibilities and limitations of the major dark energy probes has evolved; here we summarize the major probes and their crucial challenges. On the theoretical side, the taxonomy of explanations for the accelerated expansion rate is better understood, providing clear guidance to the relevant observables. We argue that: i) improving statistical precision and systematic control by taking more data, supporting research efforts to address crucial challenges for each probe, using complementary methods, and relying on cross-correlations is well motivated; ii) blinding of analyses is difficult but ever more important; iii) studies of dark energy and modified gravity are related; and iv) it is crucial that R&D for a vibrant dark energy program in the 2030s be started now by supporting studies and technical R&D that will allow embryonic proposals to mature. Understanding dark energy, arguably the biggest unsolved mystery in both fundamental particle physics and cosmology, will remain one of the focal points of cosmology in the forthcoming decade., 5 pages + references; science white paper submitted to the Astro2020 decadal survey

Published
2019

30. Cosmological Synergies Enabled by Joint Analysis of Multi-probe data from WFIRST, Euclid, and LSST

Author

Rhodes, Jason, Alonso, David, Ansarinejad, Behzad, Armstrong, Robert, Asorey, Jacobo, Avelino, Arturo, Blazek, Jonathan, Castander, Francisco J., Chary, Ranga Ram, Chen, Xingang, Choi, Ami, Clowe, Douglas, Cohen-Tanugi, Johann, Comparat, Johan, Croft, Rupert A. C., Doré, Olivier, Escoffier, Stephanie, Foley, Ryan, Fosalba, Pablo, Gruen, Daniel, Gupta, Nikhel, GUZZO, Luigi, Hawken, Adam J., Hemmati, Shoubaneh, Heitmann, Katrin, Hernquist, Lars, Heymans, Catherine, Hirata, Christopher M., Hoekstra, Henk, Huterer, Dragan, Iliev, Ilian T., Jain, Bhuvnesh, Jha, Saurabh W., Keeley, Ryan E., Kiessling, Alina, Kitching, Thomas, Koekemoer, Anton, Koushiappas, Savvas M., Kovetz, Ely D., Kruk, Jeff, L'Huillier, Benjamin, Lahav, Ofer, Lemos, Pablo, Macorra, Axel de la, Malagón, Andrés Plazas, Mandelbaum, Rachel, Masters, Daniel, McQuinn, Matthew, Melchior, Peter, Miyatake, Hironao, Newman, Jeffrey A., Nichol, Robert, Niz, Gustavo, O'Connor, Paul, Penna-Lima, Mariana, Percival, Will J., Perlmutter, Saul, Pisani, Alice, Rigault, Mickael, Rossi, Graziano, Schmittfull, Marcel, Schuhmann, Robert, Scolnic, Dan, Sereno, Mauro, Shan, Huanyuan, Shirasaki, Masato, Simon, Sara, Slosar, Anže, Spergel, David, Sridhar, Srivatsan, Takada, Masahiro, Troxel, M. A., Wang, Yun, Weinberg, David, Yoshida, Naoki, Zhang, Yuanyuan, and LSST Dark Energy Science Collaboration

Abstract

WFIRST, Euclid, and LSST are all missions designed to perform dedicated cosmology surveys that offer unprecedented statistical constraining power and control of systematic uncertainties. There is a growing realization that these missions will be significantly more powerful when the data are processed and analyzed in unison.

Published
2019

31. Scratches from the Past: Inflationary Archaeology through Features in the Power Spectrum of Primordial Fluctuations

Author

Slosar, Anze, Abazajian, Kevork N., Abidi, Muntazir, Adshead, Peter, Ahmed, Zeeshan, Alonso, David, Amin, Mustafa A., Ansarinejad, Behzad, Armstrong, Robert, Baccigalupi, Carlo, Bandura, Kevin, Battaglia, Nicholas, Bleem, Lindsey, Bond, J. Richard, Borrill, Julian, Bouchet, François R., Bull, Philip, Byrnes, Christian T., Carlstrom, John E., Castorina, Emanuele, Challinor, Anthony, Chen, Xingang, Cohn, J. D., Cooray, Asantha, Cyr-Racine, Francis-Yan, Demarteau, Marcel, Doré, Olivier, Douglass, Kelly A., Yutong, Duan, Dvorkin, Cora, Ellison, John, Essinger-Hileman, Tom, Fabbian, Giulio, Ferraro, Simone, Flauger, Raphael, Font-Ribera, Andreu, Foreman, Simon, García-Bellido, Juan, Gerbino, Martina, Gluscevic, Vera, Gontcho, A., Górski, Krzysztof M., Green, Daniel, Gudmundsson, Jon E., Gupta, Nikhel, Hanany, Shaul, Handley, Will, Hill, J. Colin, Hložek, Renée, Horiuchi, Shunsaku, Huterer, Dragan, Ishak, Mustapha, Johnson, Bradley, Kamionkowski, Marc, Karkare, Kirit S., Keeley, Ryan E., Khatri, Rishi, Kisner, Theodore, Kneib, Jean-Paul, Knox, Lloyd, Koushiappas, Savvas M., Kovetz, Ely D., Kazuya Koyama, Lahav, Ofer, Lattanzi, Massimiliano, Lee, Hayden, Liguori, Michele, Loverde, Marilena, Martini, Paul, Masui, Kiyoshi, Mcallister, Liam, Mcmahon, Jeff, Daniel Meerburg, P., Meyers, Joel, Motloch, Pavel, Mukherjee, Suvodip, Muñoz, Julian B., Myers, Adam D., Nagy, Johanna, Newburgh, Laura, Niemack, Michael D., Niz, Gustavo, Nomerotski, Andrei, Page, Lyman, Palma, Gonzalo A., Penna-Lima, Mariana, Percival, Will J., Piacentini, Francesco, Pierpaoli, Elena, Pogosian, Levon, Prakash, Abhishek, Pryke, Clement, Puglisi, Giuseppe, Stompor, Radek, Raveri, Marco, Ross, Ashley J., Rossi, Graziano, Ruhl, John, Samushia, Lado, Sasaki, Misao, Schaan, Emmanuel, Schillaci, Alessandro, Schmittfull, Marcel, Sehgal, Neelima, Senatore, Leonardo, Seo, Hee-Jong, Shafieloo, Arman, Shan, Huanyuan, Sherwin, Blake D., Silverstein, Eva, Simon, Sara, Starkman, Glenn, Suzuki, Aritoki, Switzer, Eric R., Basu Thakur, Ritoban, Timbie, Peter, Tolley, Andrew J., Tristram, Matthieu, Trodden, Mark, Umiltà, Caterina, Di Valentino, Eleonora, Vargas-Magaña, M., Vieregg, Abigail, Wallisch, Benjamin, Wands, David, Wang, Yi, Watson, Scott, Whitehorn, Nathan, Wu, W. L. K., Xianyu, Zhong-Zhi, Xu, Weishuang, Xu, Zhilei, Yasini, Siavash, Zaldarriaga, Matias, Zhao, Gong-Bo, Zhu, Ningfeng, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
High Energy Physics - Theory, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], hep-th, fluctuation: primordial, FOS: Physical sciences, hep-ph, Astrophysics::Cosmology and Extragalactic Astrophysics, cosmic background radiation, inflation: model, power spectrum: primordial, inflation: nonminimal, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), High Energy Physics - Theory (hep-th), [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], astro-ph.CO, structure, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Inflation may provide unique insight into the physics at the highest available energy scales that cannot be replicated in any realistic terrestrial experiment. Features in the primordial power spectrum are generically predicted in a wide class of models of inflation and its alternatives, and are observationally one of the most overlooked channels for finding evidence for non-minimal inflationary models. Constraints from observations of the cosmic microwave background cover the widest range of feature frequencies, but the most sensitive constraints will come from future large-scale structure surveys that can measure the largest number of linear and quasi-linear modes., Comment: 5 pages + references, 1 figure; science white paper submitted to the Astro2020 decadal survey

Published
2019

32. The Massive and Distant Clusters of WISE Survey. VI. Stellar Mass Fractions of a Sample of High-redshift Infrared-selected Clusters

Author

Decker, Bandon, primary, Brodwin, Mark, additional, Abdulla, Zubair, additional, Gonzalez, Anthony H., additional, Marrone, Daniel P., additional, O’Donnell, Christine, additional, Stanford, S. A., additional, Wylezalek, Dominika, additional, Carlstrom, John E., additional, Eisenhardt, Peter R. M., additional, Mantz, Adam, additional, Mo, Wenli, additional, Moravec, Emily, additional, Stern, Daniel, additional, Aldering, Greg, additional, Ashby, Matthew L. N., additional, Boone, Kyle, additional, Hayden, Brian, additional, Gupta, Nikhel, additional, and McDonald, Michael A., additional

Published
2019
Full Text
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33. High frequency cluster radio galaxies and the Sunyaev-Zel’dovich Effect properties of galaxy clusters

Author

Gupta, Nikhel

Subjects
FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxies, Galaxy Clusters, Luminosity function, Mass function, Submillimeter galaxies, Cosmology, Observations, Simulations, Astrophysics::Galaxy Astrophysics
Abstract

The high frequency mm-wave surveys by the South Pole Telescope (SPT), the Atacama Cosmology Telescope (ACT), and Planck have enabled the Sunyaev-Zel’dovich Effect (SZE) detection of large cluster samples and their use to constrain cosmological parameters. In these analyses the connection between the cluster SZE signature and the underlying halo mass described by the so-called observable-mass relation plays a central role. A calibration of this relation requires robust masses determined through the use of galaxy dynamics or weak gravitational lensing, whose biases can be calibrated using current structure formation simulations. Groups like the Planck collaboration that have attempted to employ masses derived using the assumption of Hydro-static Equilibrium (HSE) have found that their cosmological constraints are limited by the inaccuracy of this assumption. The cluster cosmology is also highly dependent on an understanding of the selection function, which in the SZE case can be impacted by radio emission from Active Galactic Nuclei (AGN) within the clusters. Although the high frequency SZE surveys listed above are working in a regime where radio AGN with sufficient flux to impact the SZE signature are rare, it it nevertheless important to study the luminosity functions of these cluster radio AGN to constrain their impact on incompleteness in SZE selected cluster samples. To begin with, we study the overdensity of point sources in the direction of X-ray- selected galaxy clusters from the Meta-Catalog of X-ray detected Clusters of galaxies (MCXC; ⟨z⟩ = 0.14) at SPT and Sydney University Molonglo Sky Survey (SUMSS) frequencies. Flux densities at 95, 150 and 220 GHz are extracted from the 2500 deg2 SPT-SZ survey maps at the locations of SUMSS sources, producing a multi-frequency catalog of radio galaxies. In the direction of massive galaxy clusters, the radio galaxy flux densities at 95 and 150 GHz are biased low by the cluster SZE signal, which is negative at these frequencies. We employ a cluster SZE model to remove the expected flux bias and then study these corrected source catalogs. We find that the high frequency radio galaxies are centrally concentrated within the clusters and that their luminosity functions (LFs) exhibit amplitudes that are characteristically an order of magnitude lower than the cluster LF at 843 MHz. We use the 150 GHz LF to estimate the impact of cluster radio galaxies on an SPT-SZ like survey. The radio galaxy flux typically produces a small bias on the SZE signal and has negligible impact on the observed scatter in the SZE mass-observable relation. If we assume there is no redshift evolution in the radio galaxy LF then 1.8 ± 0.7 percent of the clusters with detection significance ξ ≥ 4.5 would be lost from the sample. We note that with the MCXC sample we cannot place strong constraints on the redshift evolution of the high frequency radio galaxy LF. The most recent catalog of galaxy clusters for this purpose is constructed from the Dark Energy Survey first year observations (DES-Y1). Thus, we study the redshift and mass trends for the radio sources in the direction of optically selected catalog of galaxy clusters from DES. We measure luminosity functions (LFs) and Halo Occupation Numbers (HONs) for these radio sources by statistically correcting for the background population and effectively placing the radio sources at the redshift of clusters for all frequencies. We find that the number of sources depend on the cluster mass as N ∝ M^{B_H} with B_H = 0.83 ± 0.05, 0.92 ± 0.25 and 1.23 ± 0.15 for 0.843, 95 and 150 GHz datasets, respectively. The pure density evolution in LFs is estimated as (1+z)^{γ_D} , with power index γ_D = 2.32 ± 0.40, 6.68 ± 3.25 and 6.26 ± 2.60 at 0.843, 95 and 150 GHz, respectively. We repeat our exercise to estimate the sample incompleteness and bias in the observable-mass relation for 2500 deg2 of SPT- SZ like survey. We find that 10.7 ± 2.4 percent of the clusters would be lost from the cluster sample with detection significance ξ ≥ 5 and redshift range 0.25 < z < 1.55 due to radio source contamination. We are exploring the impact of the incompleteness on the cosmological parameters, and we expect that there could be some super-statistical shift in the best fit parameters, because the Poisson noise on the full cluster sample in the latest analysis is at the 5 percent level. We also explore the impact of the radio galaxy contamination on the observable–mass relation, finding that the shift in the parameters of the relation is well within the statistical uncertainties derived for these parameters in the most recent cosmological analysis; thus, it is not an important systematic for cosmological parameter estimation using cluster abundance. Moreover, in our cluster cosmology analysis approach we empirically calibrate the observable–mass relation, and therefore our approach is insensitive to this effect. In the past few years a lot of attention is offered towards investigations of the galaxy cluster observable-mass scaling relations. One method is to measure the mass from X- ray observations of the ICM combined with the assumption of HSE and to calibrate the observable-mass relation using these HSE masses. However, given that galaxy clusters are young objects still actively growing through accretion, it is unlikely that HSE pertains in these systems – particularly those systems having undergone recent major mergers. Thus, using these masses will produce misleading conclusions about the observable-mass scaling relation. It is important to quantify these systematics in the framework where true mass of cluster is known. We present a detailed study of the galaxy cluster thermal SZE signal Y and pressure profiles using Magneticum Pathfinder hydrodynamical simulations. With a sample of 50,000 galaxy clusters (M500c > 1.4 × 10^14 M⊙) out to z = 2, we find significant variations in the shape of the pressure profile with mass and redshift and present a new generalized NFW model that follows these trends. We show that the thermal pressure at R500c accounts for only 80 percent of the pressure required to maintain hydrostatic equilibrium, and therefore even idealized hydrostatic mass estimates would be biased at the 20 percent level. We compare the cluster SZE signal extracted from a sphere with different virial-like radii, a virial cylinder within a narrow redshift slice and the full light cone, confirming small scatter (σ_{ln Y} ≃ 0.087) in the sphere and showing that structure immediately surrounding clusters increases the scatter and strengthens non self-similar redshift evolution in the cylinder. Uncorrelated large scale structure along the line of sight leads to an increase in the SZE signal and scatter that is more pronounced for low mass clusters, resulting in non self-similar trends in both mass and redshift and a mass dependent scatter that is ~ 0.16 at low masses. The scatter distribution is consistent with log-normal in all cases. We present a model of the offsets between the center of the gravitational potential and the SZE center that follows the variations with cluster mass and redshift., Die Hochfrequenz-Millimeterwellen Durchmusterungen durch das South Pole Telescope (SPT), das Atacama Cosmology Telescope (ACT) und der ESA Satellitenmission Planck ermo ̈glichen die Sunyaev-Zeldovitsch-Effekt-Detektion (SZE) grosser Galaxienhaufenkata- loge und deren Nutzung zur Bestimmung der kosmologischen Parameter. Das Verha ̈ltnis des SZE Signals zur zugrundeliegenden Halonenmasses des Galaxienhaufens - die soge- nannte mass-observable relation - ist von zentraler Bedeutung fu ̈r diese Untersuchungen. Die Bestimmung der kosmologischen Parameter ist insbesondere stark von der Annahme des hydrostatischen Gleichgewichts (hydrostatic equilibrium, HSE) abha ̈ngig. Mit Hilfe der hydrodynamischen Magneticum Pathfinder Simulationen bestimmen wir anhand eines simulierten Galaxienhaufenkataloges die Abha ̈ngigkeit des Druckprofiles von der Halonen- masse und der Rotverschiebung des Haufens. Wir weisen nach, dass der thermische Druck nur 80Neben der mass-observable relation ha ̈ngt die Bestimmung der kosmologischen Pa- rameter durch Galaxienhaufenkataloge auch von der Selektion der Kataloge ab. Insbeson- dere kann die Anwesenheit von punktfo ̈rmigen Radioquellen in einem Galaxienhaufen zu einer Verringerung des SZE Signals, und folglich einer Nichtdetektion, fu ̈hren. Um den Ein- fluss dieses Effekts auf die Anzahl Haufen im SPT-Katalog zu bestimmen, untersuchen wir die Ha ̈ufigkeit von punktfo ̈rmigen Radioquellen in einem Ro ̈ntgen- und einem optisch se- lektiertem Haufenkatalog. Wir bestimmen die Leuchtkraftverteilung (luminosity function) der Radioquellen, und untersuchen dessen Entwicklung mit Rotverschiebung. Die daraus folgende Anzahl nichtdetektierter Quellen ist kleiner als der Poissonfehler auf der Anzahl Haufen im SPT-Katalog, und fu ̈hrt somit zu keiner signifikanten Fehlbestimmung der kos- mologischen Parameter. Zusammenfassend stellen wir fest, dass die Galaxienhaufenselek- tion durch den SZE Effekt eine ausreichende Vollsta ̈ndigkeit der Kataloge sicherstellt. Die Annahme von HSE fu ̈hrt jedoch zu einer 20-prozentigen Fehlscha ̈tzung der Halonenmassen der Haufen. Anhand unserer Arbeit kann diese Fehlscha ̈tzung kalibriert und korrigiert werden.

Published
2018
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34. Performance and characterization of the SPT-3G digital frequency-domain multiplexed readout system using an improved noise and crosstalk model

Author

Montgomery, Joshua, Ade, Peter A. R., Ahmed, Zeeshan, Anderes, Ethan, Anderson, Adam J., Archipley, Melanie, Avva, Jessica S., Aylor, Kevin, Balkenhol, Lennart, Barry, Peter S., Thakur, Ritoban B., Benabed, Karim, Bender, Amy N., Benson, Bradford A., Bianchini, Federico, Bleem, Lindsey E., Bouchet, Francois R., Bryant, Lincoln, Byrum, Karen, Carlstrom, John E., Carter, Faustin W., Cecil, Thomas W., Chang, Clarence L., Chaubal, Prakrut, Chen, Geoffrey, Cho, Hsiaomei, Chou, Ti-Lin, Cliche, Jean-Francois, Crawford, Tom M., Cukierman, Ari, Daley, Cail, de Haan, Tijmen, Denison, Edward V., Dibert, Karia, Ding, Junjia, Dobbs, Matt A., Dutcher, Daniel, Elleflot, Tucker, Everett, Wendeline, Feng, Cahng, Ferguson, Kyle R., Foster, Allen, Fu, Jianyang, Galli, Silvia, Gambrel, Anne E., Gardner, Robert W., Goeckner-Wald, Neil, Groh, John C., Gualtieri, Riccardo, Guns, Sam, Gupta, Nikhel, Guyser, Robert, Halverson, Nils W., Harke-Hosemann, Angelina H., Harrington, Nicholas L., Henning, Jason W., Hilton, Gene C., Hivon, Eric, Holzapfel, William L., Hood, John C., Howe, Doug, Huang, Nicholas, Irwin, Kent D., Jeong, Oliver B., Jonas, Michelle, Jones, Adam, Khaire, Trupti S., Knox, Lloyd, Kofman, Anna M., Korman, Milo, Kubik, Donna L., Kuhlmann, Stephen, Kuo, Chao-Lin, Lee, Adrian T., Leitch, Erik M., Lowitz, Amy E., Lu, Chunyu, Meyer, Stephan S., Michalik, Daniel, Millea, Marius, Nadolski, Andrew, Natoli, Tyler, Nguyen, Hogan, Noble, Gavin I., Novosad, Valentine, Omori, Yuuki, Padin, Steve, Pan, Zhaodi, Paschos, Pascal, Pearson, John, Posada, Chrystian M., Prabhu, Karthik, Quan, Wei, Rahlin, Alexandra, Reichardt, Christian L., Riebel, David, Riedel, Benedikt, Rouble, Maclean, Ruhl, John E., Sayre, James T., Schiappucci, Eduardo, Shirokoff, Erik, Smecher, Graeme, Sobrin, Joshua A., Stark, Antony A., Stephen, Judith, Story, Kyle T., Suzuki, Aritoki, Thompson, Keith L., Thorne, Ben, Tucker, Carole, Umilta, Caterina, Vale, Leila R., Vanderlinde, Keith, Vieira, Joaquin D., Wang, Gensheng, Whitehorn, Nathan, Wu, Wai L. K., Yefremenko, Volodymyr, Yoon, Ki W., and Young, Matt R.

Published
2021
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35. Astro2020 Science White Paper: Cosmological Synergies Enabled by Joint Analysis of Multi-probe data from WFIRST, Euclid, and LSST

Author

Rhodes, Jason, Alonso, David, Ansarinejad, Behzad, Armstrong, Robert, Asorey, Jacobo, Avelino, Arturo, Blazek, Jonathan, Castander, Francisco J., Chary, Ranga Ram, Chen, Xingang, Choi, Ami, Clowe, Douglas, Cohen-Tanugi, Johann, Comparat, Johan, Croft, Rupert A. C., Doré, Olivier, Escoffier, Stephanie, Foley, Ryan, Fosalba, Pablo, Gruen, Daniel, Gupta, Nikhel, Guzzo, Luigi, Hawken, Adam J., Hemmati, Shoubaneh, Heitmann, Katrin, Hernquist, Lars, Heymans, Catherine, Hirata, Christopher M., Hoekstra, Henk, Huterer, Dragan, Iliev, Ilian T., Jain, Bhuvnesh, Jha, Saurabh W., Keeley, Ryan E., Kiessling, Alina, Kitching, Thomas, Koekemoer, Anton, Koushiappas, Savvas M., Kovetz, Ely D., Kruk, Jeff, L Huillier, Benjamin, Lahav, Ofer, Pablo Lemos, La Macorra, Axel, Plazas Malagón, Andrés, Mandelbaum, Rachel, Masters, Daniel, Mcquinn, Matthew, Melchior, Peter, Miyatake, Hironao, Newman, Jeffrey A., Nichol, Robert, Niz, Gustavo, O Connor, Paul, Penna-Lima, Mariana, Percival, Will J., Perlmutter, Saul, Pisani, Alice, Rigault, Mickael, Rossi, Graziano, Schmittfull, Marcel, Schuhmann, Robert, Scolnic, Dan, Sereno, Mauro, Shan, Huanyuan, Shirasaki, Masato, Simon, Sara, Slosar, Anže, Spergel, David, Sridhar, Srivatsan, Takada, Masahiro, Troxel, M. A., Wang, Yun, Weinberg, David, Yoshida, Naoki, Zhang, Yuanyuan, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Durham University, Lawrence Livermore National Laboratory (LLNL), Korea Astronomy and Space Science Institute (KASI), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, Ecole Polytechnique Fédérale de Lausanne (EPFL), Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Infrared Processing and Analysis Center (IPAC), California Institute of Technology (CALTECH), Ohio State University [Columbus] (OSU), Laboratoire Univers et Particules de Montpellier (LUPM), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Carnegie Mellon University [Pittsburgh] (CMU), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), University of California [Santa Cruz] (UC Santa Cruz), University of California (UC), Kavli Institute for Particle Astrophysics and Cosmology (KIPAC), Stanford University, University of Melbourne, Dipartimento di Fisica (Milano), Università degli Studi di Milano = University of Milan (UNIMI), Argonne National Laboratory [Lemont] (ANL), Royal Observatory Edinburgh (ROE), University of Edinburgh, Leiden Observatory [Leiden], Universiteit Leiden, University of Sussex, University of Pennsylvania, Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Space Telescope Science Institute (STSci), Brown University, Ben-Gurion University of the Negev (BGU), NASA Goddard Space Flight Center (GSFC), Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM), Princeton University, Nagoya University, Department of Physics and Astronomy [Pittsburgh], University of Pittsburgh (PITT), Pennsylvania Commonwealth System of Higher Education (PCSHE)-Pennsylvania Commonwealth System of Higher Education (PCSHE), University of Portsmouth, Universidad de Guanajuato, Brookhaven National Laboratory [Upton, NY] (BNL), UT-Battelle, LLC-Stony Brook University [SUNY] (SBU), State University of New York (SUNY)-State University of New York (SUNY)-U.S. Department of Energy [Washington] (DOE), Universidade de Brasilia [Brasília] (UnB), University of Waterloo [Waterloo], Perimeter Institute for Theoretical Physics [Waterloo], Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy and Space Science [Sejong University], Sejong University, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Duke University [Durham], Dipartimento di Fisica, Politecnico di Torino = Polytechnic of Turin (Polito), Shanghai Astronomical Observatory [Shanghai] (SHAO), Chinese Academy of Sciences [Beijing] (CAS), National Astronomical Observatory of Japan (NAOJ), Flatiron Institute, Simons Foundation, Korea Internet Security Agency (KISA), Institute for the Physics and Mathematics of the Universe (IPMU), The University of Tokyo (UTokyo), Fermilab Center for Particle Astrophysics, Fermi National Accelerator Laboratory (Fermilab), Okayama University, Smithsonian Institution-Harvard University [Cambridge], Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), University of California [Santa Cruz] (UCSC), University of California, Università degli Studi di Milano [Milano] (UNIMI), Universiteit Leiden [Leiden], University of Pennsylvania [Philadelphia], Universidad Nacional Autónoma de México (UNAM), U.S. Department of Energy [Washington] (DOE)-UT-Battelle, LLC-Stony Brook University [SUNY] (SBU), State University of New York (SUNY)-State University of New York (SUNY), Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), and HEP, INSPIRE

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.GRQC] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; NASA, NSF, and DOE will collectively spend well over $4B this decade and the next on missions and surveys that have dark energy cosmology as one of their primary drivers. WFIRST, Euclid, and LSST are all missions designed to perform dedicated surveys that offer unprecedented statistical constraining power and control of systematic uncertainties. However, there is a growing realization that these missions will be significantly more powerful when the data are processed and analyzed in unison. This will require coordinated cross-survey and interagency effort. With proper attention to how data are jointly processed and analyzed, the combination of these missions will provide constraints and systematics control that is better than the sum of their individual parts, as stated in the title of Jain, et al. (2015). We advocate for the three relevant US agencies to work together with our international partners to ensure that the synergy from these multi-probe missions is fully realized.

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