%0 Generic %1 thyagarajan2020detection %A Thyagarajan, Nithyanandan %A Carilli, Chris L. %A Nikolic, Bojan %A Kent, James %A Mesinger, Andrei %A Kern, Nicholas S. %A Bernardi, Gianni %A Matika, Siyanda %A Abdurashidova, Zara %A Aguirre, James E. %A Alexander, Paul %A Ali, Zaki S. %A Balfour, Yanga %A Beardsley, Adam P. %A Billings, Tashalee S. %A Bowman, Judd D. %A Bradley, Richard F. %A Burba, Jacob %A Carey, Steve %A Cheng, Carina %A DeBoer, David R. %A Dexter, Matt %A Acedo, Eloy de Lera %A Dillon, Joshua S. %A Ely, John %A Ewall-Wice, Aaron %A Fagnoni, Nicolas %A Fritz, Randall %A Furlanetto, Steven R. %A Gale-Sides, Kingsley %A Glendenning, Brian %A Gorthi, Deepthi %A Greig, Bradley %A Grobbelaar, Jasper %A Halday, Ziyaad %A Hazelton, Bryna J. %A Hewitt, Jacqueline N. %A Hickish, Jack %A Jacobs, Daniel C. %A Julius, Austin %A Kerrigan, Joshua %A Kittiwisit, Piyanat %A Kohn, Saul A. %A Kolopanis, Matthew %A Lanman, Adam %A La Plante, Paul %A Lekalake, Telalo %A Lewis, David %A Liu, Adrian %A MacMahon, David %A Malan, Lourence %A Malgas, Cresshim %A Maree, Matthys %A Martinot, Zachary E. %A Matsetela, Eunice %A Molewa, Mathakane %A Morales, Miguel F. %A Mosiane, Tshegofalang %A Neben, Abraham R. %A Parsons, Aaron R. %A Patra, Nipanjana %A Pieterse, Samantha %A Pober, Jonathan C. %A Razavi-Ghods, Nima %A Ringuette, Jon %A Robnett, James %A Rosie, Kathryn %A Sims, Peter %A Smith, Craig %A Syce, Angelo %A Williams, Peter K. G. %A Zheng, Haoxuan %D 2020 %K library %T Detection of Cosmic Structures using the Bispectrum Phase. II. First Results from Application to Cosmic Reionization Using the Hydrogen Epoch of Reionization Array %U http://arxiv.org/abs/2005.10275 %X Characterizing the epoch of reionization (EoR) at $z6$ via the redshifted 21 cm line of neutral Hydrogen (HI) is critical to modern astrophysics and cosmology, and thus a key science goal of many current and planned low-frequency radio telescopes. The primary challenge to detecting this signal is the overwhelmingly bright foreground emission at these frequencies, placing stringent requirements on the knowledge of the instruments and inaccuracies in analyses. Results from these experiments have largely been limited not by thermal sensitivity but by systematics, particularly caused by the inability to calibrate the instrument to high accuracy. The interferometric bispectrum phase is immune to antenna-based calibration and errors therein, and presents an independent alternative to detect the EoR HI fluctuations while largely avoiding calibration systematics. Here, we provide a demonstration of this technique on a subset of data from the Hydrogen Epoch of Reionization Array (HERA) to place approximate constraints on the IGM brightness temperature. From this limited data, at $z=7.7$ we infer "$1\sigma$" upper limits on the IGM brightness temperature to be $316$ "pseudo" mK at $\kappa_\parallel=0.33\,"pseudo"\,h$ Mpc$^-1$ (data-limited) and $1000$ "pseudo" mK at $\kappa_\parallel=0.875\,"pseudo"\,h$ Mpc$^-1$ (noise-limited). The "pseudo" units denote only an approximate and not an exact correspondence to the actual distance scales and brightness temperatures. By propagating models in parallel to the data analysis, we confirm that the dynamic range required to separate the cosmic HI signal from the foregrounds is similar to that in standard approaches, and the power spectrum of the bispectrum phase is still data-limited (at $10^6$ dynamic range) indicating scope for further improvement in sensitivity as the array build-out continues.

@misc{thyagarajan2020detection, abstract = {Characterizing the epoch of reionization (EoR) at $z\gtrsim 6$ via the redshifted 21 cm line of neutral Hydrogen (HI) is critical to modern astrophysics and cosmology, and thus a key science goal of many current and planned low-frequency radio telescopes. The primary challenge to detecting this signal is the overwhelmingly bright foreground emission at these frequencies, placing stringent requirements on the knowledge of the instruments and inaccuracies in analyses. Results from these experiments have largely been limited not by thermal sensitivity but by systematics, particularly caused by the inability to calibrate the instrument to high accuracy. The interferometric bispectrum phase is immune to antenna-based calibration and errors therein, and presents an independent alternative to detect the EoR HI fluctuations while largely avoiding calibration systematics. Here, we provide a demonstration of this technique on a subset of data from the Hydrogen Epoch of Reionization Array (HERA) to place approximate constraints on the IGM brightness temperature. From this limited data, at $z=7.7$ we infer "$1\sigma$" upper limits on the IGM brightness temperature to be $\le 316$ "pseudo" mK at $\kappa_\parallel=0.33\,\textrm{"pseudo"}\,h$ Mpc$^{-1}$ (data-limited) and $\le 1000$ "pseudo" mK at $\kappa_\parallel=0.875\,\textrm{"pseudo"}\,h$ Mpc$^{-1}$ (noise-limited). The "pseudo" units denote only an approximate and not an exact correspondence to the actual distance scales and brightness temperatures. By propagating models in parallel to the data analysis, we confirm that the dynamic range required to separate the cosmic HI signal from the foregrounds is similar to that in standard approaches, and the power spectrum of the bispectrum phase is still data-limited (at $\gtrsim 10^6$ dynamic range) indicating scope for further improvement in sensitivity as the array build-out continues.}, added-at = {2020-05-22T07:24:28.000+0200}, author = {Thyagarajan, Nithyanandan and Carilli, Chris L. and Nikolic, Bojan and Kent, James and Mesinger, Andrei and Kern, Nicholas S. and Bernardi, Gianni and Matika, Siyanda and Abdurashidova, Zara and Aguirre, James E. and Alexander, Paul and Ali, Zaki S. and Balfour, Yanga and Beardsley, Adam P. and Billings, Tashalee S. and Bowman, Judd D. and Bradley, Richard F. and Burba, Jacob and Carey, Steve and Cheng, Carina and DeBoer, David R. and Dexter, Matt and Acedo, Eloy de Lera and Dillon, Joshua S. and Ely, John and Ewall-Wice, Aaron and Fagnoni, Nicolas and Fritz, Randall and Furlanetto, Steven R. and Gale-Sides, Kingsley and Glendenning, Brian and Gorthi, Deepthi and Greig, Bradley and Grobbelaar, Jasper and Halday, Ziyaad and Hazelton, Bryna J. and Hewitt, Jacqueline N. and Hickish, Jack and Jacobs, Daniel C. and Julius, Austin and Kerrigan, Joshua and Kittiwisit, Piyanat and Kohn, Saul A. and Kolopanis, Matthew and Lanman, Adam and La Plante, Paul and Lekalake, Telalo and Lewis, David and Liu, Adrian and MacMahon, David and Malan, Lourence and Malgas, Cresshim and Maree, Matthys and Martinot, Zachary E. and Matsetela, Eunice and Molewa, Mathakane and Morales, Miguel F. and Mosiane, Tshegofalang and Neben, Abraham R. and Parsons, Aaron R. and Patra, Nipanjana and Pieterse, Samantha and Pober, Jonathan C. and Razavi-Ghods, Nima and Ringuette, Jon and Robnett, James and Rosie, Kathryn and Sims, Peter and Smith, Craig and Syce, Angelo and Williams, Peter K. G. and Zheng, Haoxuan}, biburl = {https://www.bibsonomy.org/bibtex/278890664e536de3b6e3eb5f362d6e88a/gpkulkarni}, description = {Detection of Cosmic Structures using the Bispectrum Phase. II. First Results from Application to Cosmic Reionization Using the Hydrogen Epoch of Reionization Array}, interhash = {b9dafac88cf5418fc3528bc42bd426fa}, intrahash = {78890664e536de3b6e3eb5f362d6e88a}, keywords = {library}, note = {cite arxiv:2005.10275Comment: 22 pages, 12 figures (including sub-figures). Accepted for publication in PhRvD. Abstract may be slightly abridged compared to the actual manuscript due to length limitations on arXiv}, timestamp = {2020-05-22T07:24:28.000+0200}, title = {Detection of Cosmic Structures using the Bispectrum Phase. II. First Results from Application to Cosmic Reionization Using the Hydrogen Epoch of Reionization Array}, url = {http://arxiv.org/abs/2005.10275}, year = 2020 }