[{"oa_version":"Preprint","type":"journal_article","external_id":{"arxiv":["1503.06214"]},"month":"05","abstract":[{"lang":"eng","text":"Weak gravitational lensing is a powerful cosmological probe, with non--Gaussian features potentially containing the majority of the information. We examine constraints on the parameter triplet (Ωm,w,σ8) from non-Gaussian features of the weak lensing convergence field, including a set of moments (up to 4th order) and Minkowski functionals, using publicly available data from the 154deg2 CFHTLenS survey. We utilize a suite of ray--tracing N-body simulations spanning 91 points in (Ωm,w,σ8) parameter space, replicating the galaxy sky positions, redshifts and shape noise in the CFHTLenS catalogs. We then build an emulator that interpolates the simulated descriptors as a function of (Ωm,w,σ8), and use it to compute the likelihood function and parameter constraints. We employ a principal component analysis to reduce dimensionality and to help stabilize the constraints with respect to the number of bins used to construct each statistic. Using the full set of statistics, we find Σ8≡σ8(Ωm/0.27)^0.55=0.75±0.04 (68% C.L.), in agreement with previous values. We find that constraints on the (Ωm,σ8) doublet from the Minkowski functionals suffer a strong bias. However, high-order moments break the (Ωm,σ8) degeneracy and provide a tight constraint on these parameters with no apparent bias. The main contribution comes from quartic moments of derivatives."}],"main_file_link":[{"open_access":"1","url":" https://doi.org/10.48550/arXiv.1503.06214"}],"status":"public","doi":"10.1103/physrevd.91.103511","date_published":"2015-05-15T00:00:00Z","citation":{"chicago":"Petri, Andrea, Jia Liu, Zoltán Haiman, Morgan May, Lam Hui, and Jan M. Kratochvil. “Emulating the CFHTLenS Weak Lensing Data: Cosmological Constraints from Moments and Minkowski Functionals.” <i>Physical Review D</i>. American Physical Society, 2015. <a href=\"https://doi.org/10.1103/physrevd.91.103511\">https://doi.org/10.1103/physrevd.91.103511</a>.","ista":"Petri A, Liu J, Haiman Z, May M, Hui L, Kratochvil JM. 2015. Emulating the CFHTLenS weak lensing data: Cosmological constraints from moments and Minkowski functionals. Physical Review D. 91(10), 103511.","ama":"Petri A, Liu J, Haiman Z, May M, Hui L, Kratochvil JM. Emulating the CFHTLenS weak lensing data: Cosmological constraints from moments and Minkowski functionals. <i>Physical Review D</i>. 2015;91(10). doi:<a href=\"https://doi.org/10.1103/physrevd.91.103511\">10.1103/physrevd.91.103511</a>","short":"A. Petri, J. Liu, Z. Haiman, M. May, L. Hui, J.M. Kratochvil, Physical Review D 91 (2015).","ieee":"A. Petri, J. Liu, Z. Haiman, M. May, L. Hui, and J. M. Kratochvil, “Emulating the CFHTLenS weak lensing data: Cosmological constraints from moments and Minkowski functionals,” <i>Physical Review D</i>, vol. 91, no. 10. American Physical Society, 2015.","apa":"Petri, A., Liu, J., Haiman, Z., May, M., Hui, L., &#38; Kratochvil, J. M. (2015). Emulating the CFHTLenS weak lensing data: Cosmological constraints from moments and Minkowski functionals. <i>Physical Review D</i>. American Physical Society. <a href=\"https://doi.org/10.1103/physrevd.91.103511\">https://doi.org/10.1103/physrevd.91.103511</a>","mla":"Petri, Andrea, et al. “Emulating the CFHTLenS Weak Lensing Data: Cosmological Constraints from Moments and Minkowski Functionals.” <i>Physical Review D</i>, vol. 91, no. 10, 103511, American Physical Society, 2015, doi:<a href=\"https://doi.org/10.1103/physrevd.91.103511\">10.1103/physrevd.91.103511</a>."},"article_processing_charge":"No","article_number":"103511","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","date_updated":"2024-09-25T11:29:05Z","fulldoi":"https://doi.org/10.1103/physrevd.91.103511","issue":"10","publication_status":"published","quality_controlled":"1","title":"Emulating the CFHTLenS weak lensing data: Cosmological constraints from moments and Minkowski functionals","article_type":"original","author":[{"first_name":"Andrea","full_name":"Petri, Andrea","last_name":"Petri"},{"last_name":"Liu","full_name":"Liu, Jia","first_name":"Jia"},{"last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán","first_name":"Zoltán"},{"first_name":"Morgan","full_name":"May, Morgan","last_name":"May"},{"first_name":"Lam","last_name":"Hui","full_name":"Hui, Lam"},{"full_name":"Kratochvil, Jan M.","last_name":"Kratochvil","first_name":"Jan M."}],"publisher":"American Physical Society","publication_identifier":{"issn":["1550-7998","1550-2368"]},"scopus_import":"1","date_created":"2024-09-06T08:48:07Z","_id":"17702","extern":"1","oa":1,"intvolume":"        91","year":"2015","language":[{"iso":"eng"}],"arxiv":1,"day":"15","publication":"Physical Review D","volume":91},{"oa":1,"intvolume":"        91","year":"2015","language":[{"iso":"eng"}],"arxiv":1,"day":"04","volume":91,"publication":"Physical Review D","title":"Cosmology constraints from the weak lensing peak counts and the power spectrum in CFHTLenS data","quality_controlled":"1","author":[{"full_name":"Liu, Jia","last_name":"Liu","first_name":"Jia"},{"full_name":"Petri, Andrea","last_name":"Petri","first_name":"Andrea"},{"first_name":"Zoltán","full_name":"Haiman, Zoltán","last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36"},{"full_name":"Hui, Lam","last_name":"Hui","first_name":"Lam"},{"full_name":"Kratochvil, Jan M.","last_name":"Kratochvil","first_name":"Jan M."},{"last_name":"May","full_name":"May, Morgan","first_name":"Morgan"}],"article_type":"original","publication_identifier":{"issn":["1550-7998","1550-2368"]},"publisher":"American Physical Society","scopus_import":"1","extern":"1","_id":"17710","date_created":"2024-09-06T08:54:57Z","article_processing_charge":"No","article_number":"063507","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","issue":"6","publication_status":"published","date_updated":"2024-09-25T12:03:54Z","fulldoi":"https://doi.org/10.1103/physrevd.91.063507","oa_version":"Preprint","external_id":{"arxiv":["1412.0757"]},"type":"journal_article","month":"03","abstract":[{"lang":"eng","text":"Lensing peaks have been proposed as a useful statistic, containing cosmological information from non-Gaussianities that is inaccessible from traditional two-point statistics such as the power spectrum or two-point correlation functions. Here we examine constraints on cosmological parameters from weak lensing peak counts, using the publicly available data from the 154 deg^2 CFHTLenS survey. We utilize a new suite of ray-tracing N-body simulations on a grid of 91 cosmological models, covering broad ranges of the three parameters Ωm, σ8, and w, and replicating the Galaxy sky positions, redshifts, and shape noise in the CFHTLenS observations. We then build an emulator that interpolates the power spectrum and the peak counts to an accuracy of ≤5%, and compute the likelihood in the three-dimensional parameter space (Ωm, σ8, w) from both observables. We find that constraints from peak counts are comparable to those from the power spectrum, and somewhat tighter when different smoothing scales are combined. Neither observable can constrain w without external data. When the power spectrum and peak counts are combined, the area of the error \"banana'' in the (Ωm, σ8) plane reduces by a factor of ≈2, compared to using the power spectrum alone. For a flat Λ cold dark matter model, combining both statistics, we obtain the constraint σ8(Ωm/0.27)^0.63=0.85+0.03−0.03."}],"status":"public","main_file_link":[{"open_access":"1","url":" https://doi.org/10.48550/arXiv.1412.0757"}],"doi":"10.1103/physrevd.91.063507","date_published":"2015-03-04T00:00:00Z","citation":{"mla":"Liu, Jia, et al. “Cosmology Constraints from the Weak Lensing Peak Counts and the Power Spectrum in CFHTLenS Data.” <i>Physical Review D</i>, vol. 91, no. 6, 063507, American Physical Society, 2015, doi:<a href=\"https://doi.org/10.1103/physrevd.91.063507\">10.1103/physrevd.91.063507</a>.","apa":"Liu, J., Petri, A., Haiman, Z., Hui, L., Kratochvil, J. M., &#38; May, M. (2015). Cosmology constraints from the weak lensing peak counts and the power spectrum in CFHTLenS data. <i>Physical Review D</i>. American Physical Society. <a href=\"https://doi.org/10.1103/physrevd.91.063507\">https://doi.org/10.1103/physrevd.91.063507</a>","ista":"Liu J, Petri A, Haiman Z, Hui L, Kratochvil JM, May M. 2015. Cosmology constraints from the weak lensing peak counts and the power spectrum in CFHTLenS data. Physical Review D. 91(6), 063507.","chicago":"Liu, Jia, Andrea Petri, Zoltán Haiman, Lam Hui, Jan M. Kratochvil, and Morgan May. “Cosmology Constraints from the Weak Lensing Peak Counts and the Power Spectrum in CFHTLenS Data.” <i>Physical Review D</i>. American Physical Society, 2015. <a href=\"https://doi.org/10.1103/physrevd.91.063507\">https://doi.org/10.1103/physrevd.91.063507</a>.","ama":"Liu J, Petri A, Haiman Z, Hui L, Kratochvil JM, May M. Cosmology constraints from the weak lensing peak counts and the power spectrum in CFHTLenS data. <i>Physical Review D</i>. 2015;91(6). doi:<a href=\"https://doi.org/10.1103/physrevd.91.063507\">10.1103/physrevd.91.063507</a>","short":"J. Liu, A. Petri, Z. Haiman, L. Hui, J.M. Kratochvil, M. May, Physical Review D 91 (2015).","ieee":"J. Liu, A. Petri, Z. Haiman, L. Hui, J. M. Kratochvil, and M. May, “Cosmology constraints from the weak lensing peak counts and the power spectrum in CFHTLenS data,” <i>Physical Review D</i>, vol. 91, no. 6. American Physical Society, 2015."}},{"doi":"10.1103/physrevd.90.123015","status":"public","main_file_link":[{"url":" https://doi.org/10.48550/arXiv.1409.5130","open_access":"1"}],"citation":{"short":"A. Petri, M. May, Z. Haiman, J.M. Kratochvil, Physical Review D 90 (2014).","ieee":"A. Petri, M. May, Z. Haiman, and J. M. Kratochvil, “Impact of spurious shear on cosmological parameter estimates from weak lensing observables,” <i>Physical Review D</i>, vol. 90, no. 12. American Physical Society, 2014.","ama":"Petri A, May M, Haiman Z, Kratochvil JM. Impact of spurious shear on cosmological parameter estimates from weak lensing observables. <i>Physical Review D</i>. 2014;90(12). doi:<a href=\"https://doi.org/10.1103/physrevd.90.123015\">10.1103/physrevd.90.123015</a>","ista":"Petri A, May M, Haiman Z, Kratochvil JM. 2014. Impact of spurious shear on cosmological parameter estimates from weak lensing observables. Physical Review D. 90(12), 123015.","chicago":"Petri, Andrea, Morgan May, Zoltán Haiman, and Jan M. Kratochvil. “Impact of Spurious Shear on Cosmological Parameter Estimates from Weak Lensing Observables.” <i>Physical Review D</i>. American Physical Society, 2014. <a href=\"https://doi.org/10.1103/physrevd.90.123015\">https://doi.org/10.1103/physrevd.90.123015</a>.","mla":"Petri, Andrea, et al. “Impact of Spurious Shear on Cosmological Parameter Estimates from Weak Lensing Observables.” <i>Physical Review D</i>, vol. 90, no. 12, 123015, American Physical Society, 2014, doi:<a href=\"https://doi.org/10.1103/physrevd.90.123015\">10.1103/physrevd.90.123015</a>.","apa":"Petri, A., May, M., Haiman, Z., &#38; Kratochvil, J. M. (2014). Impact of spurious shear on cosmological parameter estimates from weak lensing observables. <i>Physical Review D</i>. American Physical Society. <a href=\"https://doi.org/10.1103/physrevd.90.123015\">https://doi.org/10.1103/physrevd.90.123015</a>"},"date_published":"2014-12-30T00:00:00Z","external_id":{"arxiv":["1409.5130"]},"type":"journal_article","oa_version":"Preprint","abstract":[{"text":"Residual errors in shear measurements, after corrections for instrument systematics and atmospheric effects, can impact cosmological parameters derived from weak lensing observations. Here we combine convergence maps from our suite of ray-tracing simulations with random realizations of spurious shear. This allows us to quantify the errors and biases of the triplet (Ωm,w,σ8) derived from the power spectrum (PS), as well as from three different sets of non-Gaussian statistics of the lensing convergence field: Minkowski functionals (MF), low--order moments (LM), and peak counts (PK). Our main results are: (i) We find an order of magnitude smaller biases from the PS than in previous work. (ii) The PS and LM yield biases much smaller than the morphological statistics (MF, PK). (iii) For strictly Gaussian spurious shear with integrated amplitude as low as its current estimate of σ2sys≈10−7, biases from the PS and LM would be unimportant even for a survey with the statistical power of LSST. However, we find that for surveys larger than ≈100 deg2, non-Gaussianity in the noise (not included in our analysis) will likely be important and must be quantified to assess the biases. (iv) The morphological statistics (MF,PK) introduce important biases even for Gaussian noise, which must be corrected in large surveys. The biases are in different directions in (Ωm,w,σ8) parameter space, allowing self-calibration by combining multiple statistics. Our results warrant follow-up studies with more extensive lensing simulations and more accurate spurious shear estimates.","lang":"eng"}],"month":"12","publication_status":"published","issue":"12","fulldoi":"https://doi.org/10.1103/physrevd.90.123015","date_updated":"2024-09-24T08:39:41Z","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","article_processing_charge":"No","article_number":"123015","extern":"1","_id":"17623","date_created":"2024-09-05T13:52:25Z","article_type":"original","author":[{"first_name":"Andrea","full_name":"Petri, Andrea","last_name":"Petri"},{"first_name":"Morgan","last_name":"May","full_name":"May, Morgan"},{"full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman","first_name":"Zoltán"},{"full_name":"Kratochvil, Jan M.","last_name":"Kratochvil","first_name":"Jan M."}],"title":"Impact of spurious shear on cosmological parameter estimates from weak lensing observables","quality_controlled":"1","scopus_import":"1","publication_identifier":{"issn":["1550-7998","1550-2368"]},"publisher":"American Physical Society","day":"30","arxiv":1,"volume":90,"publication":"Physical Review D","intvolume":"        90","oa":1,"language":[{"iso":"eng"}],"year":"2014"},{"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","date_updated":"2024-09-25T11:33:58Z","fulldoi":"https://doi.org/10.1103/physrevd.89.023515","publication_status":"published","issue":"2","article_number":"023515","article_processing_charge":"No","date_published":"2014-01-21T00:00:00Z","citation":{"apa":"Liu, J., Haiman, Z., Hui, L., Kratochvil, J. M., &#38; May, M. (2014). Impact of magnification and size bias on the weak lensing power spectrum and peak statistics. <i>Physical Review D</i>. American Physical Society. <a href=\"https://doi.org/10.1103/physrevd.89.023515\">https://doi.org/10.1103/physrevd.89.023515</a>","mla":"Liu, Jia, et al. “Impact of Magnification and Size Bias on the Weak Lensing Power Spectrum and Peak Statistics.” <i>Physical Review D</i>, vol. 89, no. 2, 023515, American Physical Society, 2014, doi:<a href=\"https://doi.org/10.1103/physrevd.89.023515\">10.1103/physrevd.89.023515</a>.","short":"J. Liu, Z. Haiman, L. Hui, J.M. Kratochvil, M. May, Physical Review D 89 (2014).","ieee":"J. Liu, Z. Haiman, L. Hui, J. M. Kratochvil, and M. May, “Impact of magnification and size bias on the weak lensing power spectrum and peak statistics,” <i>Physical Review D</i>, vol. 89, no. 2. American Physical Society, 2014.","chicago":"Liu, Jia, Zoltán Haiman, Lam Hui, Jan M. Kratochvil, and Morgan May. “Impact of Magnification and Size Bias on the Weak Lensing Power Spectrum and Peak Statistics.” <i>Physical Review D</i>. American Physical Society, 2014. <a href=\"https://doi.org/10.1103/physrevd.89.023515\">https://doi.org/10.1103/physrevd.89.023515</a>.","ama":"Liu J, Haiman Z, Hui L, Kratochvil JM, May M. Impact of magnification and size bias on the weak lensing power spectrum and peak statistics. <i>Physical Review D</i>. 2014;89(2). doi:<a href=\"https://doi.org/10.1103/physrevd.89.023515\">10.1103/physrevd.89.023515</a>","ista":"Liu J, Haiman Z, Hui L, Kratochvil JM, May M. 2014. Impact of magnification and size bias on the weak lensing power spectrum and peak statistics. Physical Review D. 89(2), 023515."},"main_file_link":[{"url":" https://doi.org/10.48550/arXiv.1310.7517","open_access":"1"}],"status":"public","doi":"10.1103/physrevd.89.023515","month":"01","abstract":[{"text":"The weak lensing power spectrum is a powerful tool to probe cosmological parameters. Additionally, lensing peak counts contain cosmological information beyond the power spectrum. Both of these statistics can be affected by the preferential selection of source galaxies in patches of the sky with high magnification, as well as by the dilution in the source galaxy surface density in such regions. If not accounted for, these biases introduce systematic errors for cosmological measurements. Here we quantify these systematic errors, using convergence maps from a suite of ray-tracing N-body simulations. At the cut-off magnitude m of on-going and planned major weak lensing surveys, the logarithmic slope of the cumulative number counts s = dlog[n(>m)]/dlog(m) is in the range 0.1 < s < 0.5. At s = 0.2, expected in the I band for LSST, the inferred values of Omega_m, w and sigma_8 are biased by many sigma (where sigma denotes the marginalized error) and therefore the biases will need to be carefully modeled. We also find that the parameters are biased differently in the (Omega_m, w, sigma_8) parameter space when the power spectrum and when the peak counts are used. In particular, w derived from the power spectrum is less affected than w derived from peak counts, while the opposite is true for the best-constrained combination of [sigma_8 Omega_m^gamma] (with gamma=0.62 from the power spectrum and gamma = 0.48 from peak counts). This suggests that the combination of the power spectrum and peak counts can help mitigate the impact of magnification and size biases.","lang":"eng"}],"oa_version":"Preprint","type":"journal_article","external_id":{"arxiv":["1310.7517"]},"publication":"Physical Review D","volume":89,"day":"21","arxiv":1,"year":"2014","language":[{"iso":"eng"}],"oa":1,"intvolume":"        89","date_created":"2024-09-06T08:49:04Z","_id":"17703","extern":"1","publisher":"American Physical Society","publication_identifier":{"issn":["1550-7998","1550-2368"]},"scopus_import":"1","quality_controlled":"1","title":"Impact of magnification and size bias on the weak lensing power spectrum and peak statistics","article_type":"original","author":[{"full_name":"Liu, Jia","last_name":"Liu","first_name":"Jia"},{"last_name":"Haiman","full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán"},{"first_name":"Lam","full_name":"Hui, Lam","last_name":"Hui"},{"first_name":"Jan M.","full_name":"Kratochvil, Jan M.","last_name":"Kratochvil"},{"first_name":"Morgan","full_name":"May, Morgan","last_name":"May"}]},{"issue":"2","publication_status":"published","date_updated":"2024-09-25T08:50:09Z","fulldoi":"https://doi.org/10.1103/physrevd.87.023511","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","article_number":"023511","article_processing_charge":"No","citation":{"chicago":"Yang, Xiuyuan, Jan M. Kratochvil, Kevin Huffenberger, Zoltán Haiman, and Morgan May. “Baryon Impact on Weak Lensing Peaks and Power Spectrum: Low-Bias Statistics and Self-Calibration in Future Surveys.” <i>Physical Review D</i>. American Physical Society, 2013. <a href=\"https://doi.org/10.1103/physrevd.87.023511\">https://doi.org/10.1103/physrevd.87.023511</a>.","ama":"Yang X, Kratochvil JM, Huffenberger K, Haiman Z, May M. Baryon impact on weak lensing peaks and power spectrum: Low-bias statistics and self-calibration in future surveys. <i>Physical Review D</i>. 2013;87(2). doi:<a href=\"https://doi.org/10.1103/physrevd.87.023511\">10.1103/physrevd.87.023511</a>","ista":"Yang X, Kratochvil JM, Huffenberger K, Haiman Z, May M. 2013. Baryon impact on weak lensing peaks and power spectrum: Low-bias statistics and self-calibration in future surveys. Physical Review D. 87(2), 023511.","short":"X. Yang, J.M. Kratochvil, K. Huffenberger, Z. Haiman, M. May, Physical Review D 87 (2013).","ieee":"X. Yang, J. M. Kratochvil, K. Huffenberger, Z. Haiman, and M. May, “Baryon impact on weak lensing peaks and power spectrum: Low-bias statistics and self-calibration in future surveys,” <i>Physical Review D</i>, vol. 87, no. 2. American Physical Society, 2013.","mla":"Yang, Xiuyuan, et al. “Baryon Impact on Weak Lensing Peaks and Power Spectrum: Low-Bias Statistics and Self-Calibration in Future Surveys.” <i>Physical Review D</i>, vol. 87, no. 2, 023511, American Physical Society, 2013, doi:<a href=\"https://doi.org/10.1103/physrevd.87.023511\">10.1103/physrevd.87.023511</a>.","apa":"Yang, X., Kratochvil, J. M., Huffenberger, K., Haiman, Z., &#38; May, M. (2013). Baryon impact on weak lensing peaks and power spectrum: Low-bias statistics and self-calibration in future surveys. <i>Physical Review D</i>. American Physical Society. <a href=\"https://doi.org/10.1103/physrevd.87.023511\">https://doi.org/10.1103/physrevd.87.023511</a>"},"date_published":"2013-01-14T00:00:00Z","doi":"10.1103/physrevd.87.023511","status":"public","main_file_link":[{"url":" https://doi.org/10.48550/arXiv.1210.0608","open_access":"1"}],"abstract":[{"text":"Peaks in two-dimensional weak lensing (WL) maps contain significant cosmological information, complementary to the WL power spectrum. This has recently been demonstrated using N-body simulations which neglect baryonic effects. Here we employ ray-tracing N-body simulations in which we manually steepen the density profile of each dark matter halo, mimicking the cooling and concentration of baryons into dark matter potential wells. We find, in agreement with previous works, that this causes a significant increase in the amplitude of the WL power spectrum on small scales (spherical harmonic index l>1,000). We then study the impact of the halo concentration increase on the peak counts, and find the following. (i) Low peaks (with convergence 0.02 < kappa_peak < 0.08), remain nearly unaffected. These peaks are created by a constellation of several halos with low masses (10^12-10^13 M_sun) and large angular offsets from the peak center (> 0.5 R_vir); as a result, they are insensitive to the central halo density profiles. These peaks contain most of the cosmological information, and thus provide an unusually sensitive and unbiased probe. (ii) The number of high peaks (with convergence kappa_peak > 0.08) is increased. However, when the baryon effects are neglected in cosmological parameter estimation, then the high peaks lead to a modest bias, comparable to that from the power spectrum on relatively large-scales (l<2000), and much smaller than the bias from the power spectrum on smaller scales (l>2,000). (iii) In the 3D parameter space (sigma_8, Omega_m, w), the biases from the high peaks and the power spectra are in different directions. This suggests the possibility of \"self-calibration\": the combination of peak counts and power spectrum can simultaneously constrain baryonic physics and cosmological parameters.","lang":"eng"}],"month":"01","type":"journal_article","external_id":{"arxiv":["1210.0608"]},"oa_version":"Preprint","volume":87,"publication":"Physical Review D","day":"14","arxiv":1,"language":[{"iso":"eng"}],"year":"2013","intvolume":"        87","oa":1,"extern":"1","_id":"17677","date_created":"2024-09-06T08:03:51Z","scopus_import":"1","publication_identifier":{"issn":["1550-7998","1550-2368"]},"publisher":"American Physical Society","author":[{"last_name":"Yang","full_name":"Yang, Xiuyuan","first_name":"Xiuyuan"},{"first_name":"Jan M.","full_name":"Kratochvil, Jan M.","last_name":"Kratochvil"},{"first_name":"Kevin","full_name":"Huffenberger, Kevin","last_name":"Huffenberger"},{"first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán","last_name":"Haiman"},{"full_name":"May, Morgan","last_name":"May","first_name":"Morgan"}],"article_type":"original","title":"Baryon impact on weak lensing peaks and power spectrum: Low-bias statistics and self-calibration in future surveys","quality_controlled":"1"},{"_id":"17704","date_created":"2024-09-06T08:49:55Z","extern":"1","publisher":"American Physical Society","publication_identifier":{"issn":["1550-7998","1550-2368"]},"scopus_import":"1","quality_controlled":"1","title":"Cosmology with Minkowski functionals and moments of the weak lensing convergence field","author":[{"full_name":"Petri, Andrea","last_name":"Petri","first_name":"Andrea"},{"first_name":"Zoltán","last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán"},{"full_name":"Hui, Lam","last_name":"Hui","first_name":"Lam"},{"last_name":"May","full_name":"May, Morgan","first_name":"Morgan"},{"first_name":"Jan M.","last_name":"Kratochvil","full_name":"Kratochvil, Jan M."}],"article_type":"original","publication":"Physical Review D","volume":88,"day":"05","arxiv":1,"year":"2013","language":[{"iso":"eng"}],"oa":1,"intvolume":"        88","date_published":"2013-12-05T00:00:00Z","citation":{"apa":"Petri, A., Haiman, Z., Hui, L., May, M., &#38; Kratochvil, J. M. (2013). Cosmology with Minkowski functionals and moments of the weak lensing convergence field. <i>Physical Review D</i>. American Physical Society. <a href=\"https://doi.org/10.1103/physrevd.88.123002\">https://doi.org/10.1103/physrevd.88.123002</a>","mla":"Petri, Andrea, et al. “Cosmology with Minkowski Functionals and Moments of the Weak Lensing Convergence Field.” <i>Physical Review D</i>, vol. 88, no. 12, 123002, American Physical Society, 2013, doi:<a href=\"https://doi.org/10.1103/physrevd.88.123002\">10.1103/physrevd.88.123002</a>.","ista":"Petri A, Haiman Z, Hui L, May M, Kratochvil JM. 2013. Cosmology with Minkowski functionals and moments of the weak lensing convergence field. Physical Review D. 88(12), 123002.","chicago":"Petri, Andrea, Zoltán Haiman, Lam Hui, Morgan May, and Jan M. Kratochvil. “Cosmology with Minkowski Functionals and Moments of the Weak Lensing Convergence Field.” <i>Physical Review D</i>. American Physical Society, 2013. <a href=\"https://doi.org/10.1103/physrevd.88.123002\">https://doi.org/10.1103/physrevd.88.123002</a>.","ama":"Petri A, Haiman Z, Hui L, May M, Kratochvil JM. Cosmology with Minkowski functionals and moments of the weak lensing convergence field. <i>Physical Review D</i>. 2013;88(12). doi:<a href=\"https://doi.org/10.1103/physrevd.88.123002\">10.1103/physrevd.88.123002</a>","ieee":"A. Petri, Z. Haiman, L. Hui, M. May, and J. M. Kratochvil, “Cosmology with Minkowski functionals and moments of the weak lensing convergence field,” <i>Physical Review D</i>, vol. 88, no. 12. American Physical Society, 2013.","short":"A. Petri, Z. Haiman, L. Hui, M. May, J.M. Kratochvil, Physical Review D 88 (2013)."},"main_file_link":[{"open_access":"1","url":" https://doi.org/10.48550/arXiv.1309.4460"}],"status":"public","doi":"10.1103/physrevd.88.123002","month":"12","abstract":[{"text":"We compare the efficiency of moments and Minkowski functionals (MFs) in constraining the subset of cosmological parameters (Omega_m,w,sigma_8) using simulated weak lensing convergence maps. We study an analytic perturbative expansion of the MFs in terms of the moments of the convergence field and of its spatial derivatives. We show that this perturbation series breaks down on smoothing scales below 5', while it shows a good degree of convergence on larger scales (15'). Most of the cosmological distinguishing power is lost when the maps are smoothed on these larger scales. We also show that, on scales comparable to 1', where the perturbation series does not converge, cosmological constraints obtained from the MFs are approximately 1.5-2 times better than the ones obtained from the first few moments of the convergence distribution --- provided that the latter include spatial information, either from moments of gradients, or by combining multiple smoothing scales. Including either a set of these moments or the MFs can significantly tighten constraints on cosmological parameters, compared to the conventional method of using the power spectrum alone.","lang":"eng"}],"oa_version":"Preprint","type":"journal_article","external_id":{"arxiv":["1309.4460"]},"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","fulldoi":"https://doi.org/10.1103/physrevd.88.123002","date_updated":"2024-09-25T11:35:11Z","publication_status":"published","issue":"12","article_number":"123002","article_processing_charge":"No"},{"status":"public","main_file_link":[{"url":" https://doi.org/10.48550/arXiv.1109.6334","open_access":"1"}],"doi":"10.1103/physrevd.85.103513","date_published":"2012-04-10T00:00:00Z","citation":{"apa":"Kratochvil, J. M., Lim, E. A., Wang, S., Haiman, Z., May, M., &#38; Huffenberger, K. (2012). Probing cosmology with weak lensing Minkowski functionals. <i>Physical Review D</i>. American Physical Society. <a href=\"https://doi.org/10.1103/physrevd.85.103513\">https://doi.org/10.1103/physrevd.85.103513</a>","mla":"Kratochvil, Jan M., et al. “Probing Cosmology with Weak Lensing Minkowski Functionals.” <i>Physical Review D</i>, vol. 85, no. 10, 103513, American Physical Society, 2012, doi:<a href=\"https://doi.org/10.1103/physrevd.85.103513\">10.1103/physrevd.85.103513</a>.","ieee":"J. M. Kratochvil, E. A. Lim, S. Wang, Z. Haiman, M. May, and K. Huffenberger, “Probing cosmology with weak lensing Minkowski functionals,” <i>Physical Review D</i>, vol. 85, no. 10. American Physical Society, 2012.","short":"J.M. Kratochvil, E.A. Lim, S. Wang, Z. Haiman, M. May, K. Huffenberger, Physical Review D 85 (2012).","chicago":"Kratochvil, Jan M., Eugene A. Lim, Sheng Wang, Zoltán Haiman, Morgan May, and Kevin Huffenberger. “Probing Cosmology with Weak Lensing Minkowski Functionals.” <i>Physical Review D</i>. American Physical Society, 2012. <a href=\"https://doi.org/10.1103/physrevd.85.103513\">https://doi.org/10.1103/physrevd.85.103513</a>.","ama":"Kratochvil JM, Lim EA, Wang S, Haiman Z, May M, Huffenberger K. Probing cosmology with weak lensing Minkowski functionals. <i>Physical Review D</i>. 2012;85(10). doi:<a href=\"https://doi.org/10.1103/physrevd.85.103513\">10.1103/physrevd.85.103513</a>","ista":"Kratochvil JM, Lim EA, Wang S, Haiman Z, May M, Huffenberger K. 2012. Probing cosmology with weak lensing Minkowski functionals. Physical Review D. 85(10), 103513."},"oa_version":"Preprint","type":"journal_article","external_id":{"arxiv":["1109.6334"]},"month":"04","abstract":[{"lang":"eng","text":"In this paper, we show that Minkowski Functionals (MFs) of weak gravitational lensing (WL) convergence maps contain significant non-Gaussian, cosmology-dependent information. To do this, we use a large suite of cosmological ray-tracing N-body simulations to create mock WL convergence maps, and study the cosmological information content of MFs derived from these maps. Our suite consists of 80 independent 512^3 N-body runs, covering seven different cosmologies, varying three cosmological parameters Omega_m, w, and sigma_8 one at a time, around a fiducial LambdaCDM model. In each cosmology, we use ray-tracing to create a thousand pseudo-independent 12 deg^2 convergence maps, and use these in a Monte Carlo procedure to estimate the joint confidence contours on the above three parameters. We include redshift tomography at three different source redshifts z_s=1, 1.5, 2, explore five different smoothing scales theta_G=1, 2, 3, 5, 10 arcmin, and explicitly compare and combine the MFs with the WL power spectrum. We find that the MFs capture a substantial amount of information from non-Gaussian features of convergence maps, i.e. beyond the power spectrum. The MFs are particularly well suited to break degeneracies and to constrain the dark energy equation of state parameter w (by a factor of ~ three better than from the power spectrum alone). The non-Gaussian information derives partly from the one-point function of the convergence (through V_0, the \"area\" MF), and partly through non-linear spatial information (through combining different smoothing scales for V_0, and through V_1 and V_2, the boundary length and genus MFs, respectively). In contrast to the power spectrum, the best constraints from the MFs are obtained only when multiple smoothing scales are combined."}],"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","issue":"10","publication_status":"published","fulldoi":"https://doi.org/10.1103/physrevd.85.103513","date_updated":"2024-09-25T08:41:09Z","article_processing_charge":"No","article_number":"103513","extern":"1","date_created":"2024-09-06T07:51:45Z","_id":"17675","title":"Probing cosmology with weak lensing Minkowski functionals","quality_controlled":"1","author":[{"full_name":"Kratochvil, Jan M.","last_name":"Kratochvil","first_name":"Jan M."},{"full_name":"Lim, Eugene A.","last_name":"Lim","first_name":"Eugene A."},{"first_name":"Sheng","full_name":"Wang, Sheng","last_name":"Wang"},{"first_name":"Zoltán","full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman"},{"full_name":"May, Morgan","last_name":"May","first_name":"Morgan"},{"first_name":"Kevin","full_name":"Huffenberger, Kevin","last_name":"Huffenberger"}],"article_type":"original","publication_identifier":{"issn":["1550-7998","1550-2368"]},"publisher":"American Physical Society","scopus_import":"1","day":"10","arxiv":1,"volume":85,"publication":"Physical Review D","oa":1,"intvolume":"        85","year":"2012","language":[{"iso":"eng"}]},{"main_file_link":[{"url":" https://doi.org/10.48550/arXiv.1109.6333","open_access":"1"}],"status":"public","doi":"10.1103/physrevd.84.043529","date_published":"2011-08-24T00:00:00Z","citation":{"chicago":"Yang, Xiuyuan, Jan M. Kratochvil, Sheng Wang, Eugene A. Lim, Zoltán Haiman, and Morgan May. “Cosmological Information in Weak Lensing Peaks.” <i>Physical Review D</i>. American Physical Society, 2011. <a href=\"https://doi.org/10.1103/physrevd.84.043529\">https://doi.org/10.1103/physrevd.84.043529</a>.","ama":"Yang X, Kratochvil JM, Wang S, Lim EA, Haiman Z, May M. Cosmological information in weak lensing peaks. <i>Physical Review D</i>. 2011;84(4). doi:<a href=\"https://doi.org/10.1103/physrevd.84.043529\">10.1103/physrevd.84.043529</a>","ista":"Yang X, Kratochvil JM, Wang S, Lim EA, Haiman Z, May M. 2011. Cosmological information in weak lensing peaks. Physical Review D. 84(4), 043529.","ieee":"X. Yang, J. M. Kratochvil, S. Wang, E. A. Lim, Z. Haiman, and M. May, “Cosmological information in weak lensing peaks,” <i>Physical Review D</i>, vol. 84, no. 4. American Physical Society, 2011.","short":"X. Yang, J.M. Kratochvil, S. Wang, E.A. Lim, Z. Haiman, M. May, Physical Review D 84 (2011).","apa":"Yang, X., Kratochvil, J. M., Wang, S., Lim, E. A., Haiman, Z., &#38; May, M. (2011). Cosmological information in weak lensing peaks. <i>Physical Review D</i>. American Physical Society. <a href=\"https://doi.org/10.1103/physrevd.84.043529\">https://doi.org/10.1103/physrevd.84.043529</a>","mla":"Yang, Xiuyuan, et al. “Cosmological Information in Weak Lensing Peaks.” <i>Physical Review D</i>, vol. 84, no. 4, 043529, American Physical Society, 2011, doi:<a href=\"https://doi.org/10.1103/physrevd.84.043529\">10.1103/physrevd.84.043529</a>."},"oa_version":"Preprint","type":"journal_article","external_id":{"arxiv":["1109.6333"]},"month":"08","abstract":[{"lang":"eng","text":"Recent studies have shown that the number counts of convergence peaks N(kappa) in weak lensing (WL) maps, expected from large forthcoming surveys, can be a useful probe of cosmology. We follow up on this finding, and use a suite of WL convergence maps, obtained from ray-tracing N-body simulations, to study (i) the physical origin of WL peaks with different heights, and (ii) whether the peaks contain information beyond the convergence power spectrum P_ell. In agreement with earlier work, we find that high peaks (with amplitudes >~ 3.5 sigma, where sigma is the r.m.s. of the convergence kappa) are typically dominated by a single massive halo. In contrast, medium-height peaks (~0.5-1.5 sigma) cannot be attributed to a single collapsed dark matter halo, and are instead created by the projection of multiple (typically, 4-8) halos along the line of sight, and by random galaxy shape noise. Nevertheless, these peaks dominate the sensitivity to the cosmological parameters w, sigma_8, and Omega_m. We find that the peak height distribution and its dependence on cosmology differ significantly from predictions in a Gaussian random field. We directly compute the marginalized errors on w, sigma_8, and Omega_m from the N(kappa) + P_ell combination, including redshift tomography with source galaxies at z_s=1 and z_s=2. We find that the N(kappa) + P_ell combination has approximately twice the cosmological sensitivity compared to P_ell alone. These results demonstrate that N(kappa) contains non-Gaussian information complementary to the power spectrum."}],"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","date_updated":"2024-09-25T07:25:48Z","fulldoi":"https://doi.org/10.1103/physrevd.84.043529","publication_status":"published","issue":"4","article_processing_charge":"No","article_number":"043529","_id":"17661","date_created":"2024-09-06T07:39:00Z","extern":"1","quality_controlled":"1","title":"Cosmological information in weak lensing peaks","author":[{"first_name":"Xiuyuan","full_name":"Yang, Xiuyuan","last_name":"Yang"},{"first_name":"Jan M.","last_name":"Kratochvil","full_name":"Kratochvil, Jan M."},{"last_name":"Wang","full_name":"Wang, Sheng","first_name":"Sheng"},{"first_name":"Eugene A.","last_name":"Lim","full_name":"Lim, Eugene A."},{"last_name":"Haiman","full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán"},{"full_name":"May, Morgan","last_name":"May","first_name":"Morgan"}],"article_type":"original","publisher":"American Physical Society","publication_identifier":{"issn":["1550-7998","1550-2368"]},"scopus_import":"1","day":"24","arxiv":1,"publication":"Physical Review D","volume":84,"oa":1,"intvolume":"        84","year":"2011","language":[{"iso":"eng"}]},{"title":"Probing cosmology with weak lensing peak counts","quality_controlled":"1","author":[{"full_name":"Kratochvil, Jan M.","last_name":"Kratochvil","first_name":"Jan M."},{"full_name":"Haiman, Zoltán","last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán"},{"first_name":"Morgan","full_name":"May, Morgan","last_name":"May"}],"article_type":"original","publication_identifier":{"issn":["1550-7998","1550-2368"]},"publisher":"American Physical Society","scopus_import":"1","extern":"1","_id":"17697","date_created":"2024-09-06T08:43:22Z","oa":1,"intvolume":"        81","year":"2010","language":[{"iso":"eng"}],"day":"10","arxiv":1,"volume":81,"publication":"Physical Review D","oa_version":"Preprint","type":"journal_article","external_id":{"arxiv":["0907.0486"]},"month":"02","abstract":[{"text":"We propose counting peaks in weak lensing (WL) maps, as a function of their height, to probe models of dark energy and to constrain cosmological parameters. Because peaks can be identified in two-dimensional WL maps directly, they can provide constraints that are free from potential selection effects and biases involved in identifying and determining the masses of galaxy clusters. We have run cosmological N-body simulations to produce WL convergence maps in three models with different constant values of the dark energy equation of state parameter, w=-0.8, -1, and -1.2, with a fixed normalization of the primordial power spectrum (corresponding to present-day normalizations of sigma8=0.742, 0.798, and 0.839, respectively). By comparing the number of WL peaks in 8 convergence bins in the range of -0.1 < kappa < 0.2, in multiple realizations of a single simulated 3x3 degree field, we show that the first (last) pair of models can be distinguished at the 95% (85%) confidence level. A survey with depth and area (20,000 sq. degrees), comparable to those expected from LSST, should have a factor of approx. 50 better parameter sensitivity. We find that relatively low-amplitude peaks (kappa = 0.03), which typically do not correspond to a single collapsed halo along the line of sight, account for most of this sensitivity. We study a range of smoothing scales and source galaxy redshifts (z_s). With a fixed source galaxy density of 15/arcmin^2, the best results are provided by the smallest scale we can reliably simulate, 1 arcminute, and z_s=2 provides substantially better sensitivity than z_s< 1.5.","lang":"eng"}],"status":"public","main_file_link":[{"open_access":"1","url":" https://doi.org/10.48550/arXiv.0907.0486"}],"doi":"10.1103/physrevd.81.043519","date_published":"2010-02-10T00:00:00Z","citation":{"ieee":"J. M. Kratochvil, Z. Haiman, and M. May, “Probing cosmology with weak lensing peak counts,” <i>Physical Review D</i>, vol. 81, no. 4. American Physical Society, 2010.","short":"J.M. Kratochvil, Z. Haiman, M. May, Physical Review D 81 (2010).","ista":"Kratochvil JM, Haiman Z, May M. 2010. Probing cosmology with weak lensing peak counts. Physical Review D. 81(4), 043519.","ama":"Kratochvil JM, Haiman Z, May M. Probing cosmology with weak lensing peak counts. <i>Physical Review D</i>. 2010;81(4). doi:<a href=\"https://doi.org/10.1103/physrevd.81.043519\">10.1103/physrevd.81.043519</a>","chicago":"Kratochvil, Jan M., Zoltán Haiman, and Morgan May. “Probing Cosmology with Weak Lensing Peak Counts.” <i>Physical Review D</i>. American Physical Society, 2010. <a href=\"https://doi.org/10.1103/physrevd.81.043519\">https://doi.org/10.1103/physrevd.81.043519</a>.","apa":"Kratochvil, J. M., Haiman, Z., &#38; May, M. (2010). Probing cosmology with weak lensing peak counts. <i>Physical Review D</i>. American Physical Society. <a href=\"https://doi.org/10.1103/physrevd.81.043519\">https://doi.org/10.1103/physrevd.81.043519</a>","mla":"Kratochvil, Jan M., et al. “Probing Cosmology with Weak Lensing Peak Counts.” <i>Physical Review D</i>, vol. 81, no. 4, 043519, American Physical Society, 2010, doi:<a href=\"https://doi.org/10.1103/physrevd.81.043519\">10.1103/physrevd.81.043519</a>."},"article_processing_charge":"No","article_number":"043519","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","publication_status":"published","issue":"4","fulldoi":"https://doi.org/10.1103/physrevd.81.043519","date_updated":"2024-09-25T11:14:37Z"},{"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","date_updated":"2024-09-30T09:16:05Z","fulldoi":"https://doi.org/10.1103/physrevd.78.103509","publication_status":"published","issue":"10","article_number":"103509","article_processing_charge":"No","date_published":"2008-11-10T00:00:00Z","citation":{"apa":"Fang, W., Wang, S., Hu, W., Haiman, Z., Hui, L., &#38; May, M. (2008). Challenges to the DGP model from horizon-scale growth and geometry. <i>Physical Review D</i>. American Physical Society. <a href=\"https://doi.org/10.1103/physrevd.78.103509\">https://doi.org/10.1103/physrevd.78.103509</a>","mla":"Fang, Wenjuan, et al. “Challenges to the DGP Model from Horizon-Scale Growth and Geometry.” <i>Physical Review D</i>, vol. 78, no. 10, 103509, American Physical Society, 2008, doi:<a href=\"https://doi.org/10.1103/physrevd.78.103509\">10.1103/physrevd.78.103509</a>.","ieee":"W. Fang, S. Wang, W. Hu, Z. Haiman, L. Hui, and M. May, “Challenges to the DGP model from horizon-scale growth and geometry,” <i>Physical Review D</i>, vol. 78, no. 10. American Physical Society, 2008.","short":"W. Fang, S. Wang, W. Hu, Z. Haiman, L. Hui, M. May, Physical Review D 78 (2008).","chicago":"Fang, Wenjuan, Sheng Wang, Wayne Hu, Zoltán Haiman, Lam Hui, and Morgan May. “Challenges to the DGP Model from Horizon-Scale Growth and Geometry.” <i>Physical Review D</i>. American Physical Society, 2008. <a href=\"https://doi.org/10.1103/physrevd.78.103509\">https://doi.org/10.1103/physrevd.78.103509</a>.","ama":"Fang W, Wang S, Hu W, Haiman Z, Hui L, May M. Challenges to the DGP model from horizon-scale growth and geometry. <i>Physical Review D</i>. 2008;78(10). doi:<a href=\"https://doi.org/10.1103/physrevd.78.103509\">10.1103/physrevd.78.103509</a>","ista":"Fang W, Wang S, Hu W, Haiman Z, Hui L, May M. 2008. Challenges to the DGP model from horizon-scale growth and geometry. Physical Review D. 78(10), 103509."},"main_file_link":[{"open_access":"1","url":" https://doi.org/10.48550/arXiv.0808.2208"}],"status":"public","doi":"10.1103/physrevd.78.103509","month":"11","abstract":[{"lang":"eng","text":"We conduct a Markov Chain Monte Carlo study of the Dvali-Gabadadze-Porrati self-accelerating braneworld scenario given the cosmic microwave background (CMB) anisotropy, supernovae and Hubble constant data by implementing an effective dark energy prescription for modified gravity into a standard Einstein-Boltzmann code. We find no way to alleviate the tension between distance measures and horizon-scale growth in this model. Growth alterations due to perturbations propagating into the bulk appear as excess CMB anisotropy at the lowest multipoles. In a flat cosmology, the maximum likelihood Dvali-Gabadadze-Porrati model is nominally a 5.3⁢𝜎 poorer fit than 𝛬⁢CDM. Curvature can reduce the tension between distance measures but only at the expense of exacerbating the problem with growth leading to a 4.8⁢𝜎 result that is dominated by the low multipole CMB temperature spectrum. While changing the initial conditions to reduce large-scale power can flatten the temperature spectrum, this also suppresses the large angle polarization spectrum in violation of recent results from the five-year Wilkinson Microwave Anisotropy Probe. The failure of this model highlights the power of combining growth and distance measures in cosmology as a test of gravity on the largest scales."}],"oa_version":"Preprint","type":"journal_article","external_id":{"arxiv":["0808.2208"]},"publication":"Physical Review D","volume":78,"day":"10","arxiv":1,"year":"2008","language":[{"iso":"eng"}],"oa":1,"intvolume":"        78","_id":"17762","date_created":"2024-09-06T09:49:53Z","extern":"1","publisher":"American Physical Society","publication_identifier":{"issn":["1550-7998","1550-2368"]},"scopus_import":"1","quality_controlled":"1","title":"Challenges to the DGP model from horizon-scale growth and geometry","author":[{"first_name":"Wenjuan","last_name":"Fang","full_name":"Fang, Wenjuan"},{"first_name":"Sheng","last_name":"Wang","full_name":"Wang, Sheng"},{"first_name":"Wayne","last_name":"Hu","full_name":"Hu, Wayne"},{"first_name":"Zoltán","last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán"},{"last_name":"Hui","full_name":"Hui, Lam","first_name":"Lam"},{"first_name":"Morgan","full_name":"May, Morgan","last_name":"May"}],"article_type":"original"},{"extern":"1","_id":"17724","date_created":"2024-09-06T09:11:38Z","article_type":"original","author":[{"first_name":"Bence","last_name":"Kocsis","full_name":"Kocsis, Bence"},{"full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman","first_name":"Zoltán"},{"first_name":"Kristen","last_name":"Menou","full_name":"Menou, Kristen"},{"first_name":"Zsolt","full_name":"Frei, Zsolt","last_name":"Frei"}],"title":"Premerger localization of gravitational-wave standard sirens with LISA: Harmonic mode decomposition","quality_controlled":"1","scopus_import":"1","publication_identifier":{"issn":["1550-7998","1550-2368"]},"publisher":"American Physical Society","day":"12","arxiv":1,"volume":76,"publication":"Physical Review D","intvolume":"        76","oa":1,"language":[{"iso":"eng"}],"year":"2007","doi":"10.1103/physrevd.76.022003","status":"public","main_file_link":[{"open_access":"1","url":" https://doi.org/10.48550/arXiv.astro-ph/0701629"}],"citation":{"ama":"Kocsis B, Haiman Z, Menou K, Frei Z. Premerger localization of gravitational-wave standard sirens with LISA: Harmonic mode decomposition. <i>Physical Review D</i>. 2007;76(2). doi:<a href=\"https://doi.org/10.1103/physrevd.76.022003\">10.1103/physrevd.76.022003</a>","ista":"Kocsis B, Haiman Z, Menou K, Frei Z. 2007. Premerger localization of gravitational-wave standard sirens with LISA: Harmonic mode decomposition. Physical Review D. 76(2), 022003.","chicago":"Kocsis, Bence, Zoltán Haiman, Kristen Menou, and Zsolt Frei. “Premerger Localization of Gravitational-Wave Standard Sirens with LISA: Harmonic Mode Decomposition.” <i>Physical Review D</i>. American Physical Society, 2007. <a href=\"https://doi.org/10.1103/physrevd.76.022003\">https://doi.org/10.1103/physrevd.76.022003</a>.","short":"B. Kocsis, Z. Haiman, K. Menou, Z. Frei, Physical Review D 76 (2007).","ieee":"B. Kocsis, Z. Haiman, K. Menou, and Z. Frei, “Premerger localization of gravitational-wave standard sirens with LISA: Harmonic mode decomposition,” <i>Physical Review D</i>, vol. 76, no. 2. American Physical Society, 2007.","apa":"Kocsis, B., Haiman, Z., Menou, K., &#38; Frei, Z. (2007). Premerger localization of gravitational-wave standard sirens with LISA: Harmonic mode decomposition. <i>Physical Review D</i>. American Physical Society. <a href=\"https://doi.org/10.1103/physrevd.76.022003\">https://doi.org/10.1103/physrevd.76.022003</a>","mla":"Kocsis, Bence, et al. “Premerger Localization of Gravitational-Wave Standard Sirens with LISA: Harmonic Mode Decomposition.” <i>Physical Review D</i>, vol. 76, no. 2, 022003, American Physical Society, 2007, doi:<a href=\"https://doi.org/10.1103/physrevd.76.022003\">10.1103/physrevd.76.022003</a>."},"date_published":"2007-07-12T00:00:00Z","external_id":{"arxiv":["0701629"]},"type":"journal_article","oa_version":"Preprint","abstract":[{"text":"The continuous improvement in localization errors (sky position and distance) in real time as LISA observes the gradual inspiral of a supermassive black hole (SMBH) binary can be of great help in identifying any prompt electromagnetic counterpart associated with the merger. We develop a new method, based on a Fourier decomposition of the time-dependent, LISA-modulated gravitational-wave signal, to study this intricate problem. The method is faster than standard Monte Carlo simulations by orders of magnitude. By surveying the parameter space of potential LISA sources, we find that counterparts to SMBH binary mergers with total mass M~10^5-10^7 M_Sun and redshifts z<~3 can be localized to within the field of view of astronomical instruments (~deg^2) typically hours to weeks prior to coalescence. This will allow targeted searches for variable electromagnetic counterparts as the merger proceeds, as well as monitoring of the most energetic coalescence phase. A rich set of astrophysical and cosmological applications would emerge from the identification of electromagnetic counterparts to these gravitational-wave standard sirens.","lang":"eng"}],"month":"07","publication_status":"published","issue":"2","date_updated":"2024-09-25T14:08:55Z","fulldoi":"https://doi.org/10.1103/physrevd.76.022003","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","article_processing_charge":"No","article_number":"022003"},{"year":"2007","language":[{"iso":"eng"}],"oa":1,"intvolume":"        76","volume":76,"publication":"Physical Review D","day":"12","arxiv":1,"publication_identifier":{"issn":["1550-7998","1550-2368"]},"publisher":"American Physical Society","scopus_import":"1","title":"Is modified gravity required by observations? An empirical consistency test of dark energy models","quality_controlled":"1","article_type":"original","author":[{"first_name":"Sheng","full_name":"Wang, Sheng","last_name":"Wang"},{"first_name":"Lam","full_name":"Hui, Lam","last_name":"Hui"},{"first_name":"Morgan","last_name":"May","full_name":"May, Morgan"},{"id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán","last_name":"Haiman","first_name":"Zoltán"}],"extern":"1","_id":"17783","date_created":"2024-09-06T10:16:50Z","article_number":"063503","article_processing_charge":"No","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","publication_status":"published","issue":"6","date_updated":"2024-09-30T12:45:38Z","fulldoi":"https://doi.org/10.1103/physrevd.76.063503","month":"09","abstract":[{"lang":"eng","text":"We apply the technique of parameter-splitting to existing cosmological data sets, to check for a generic failure of dark energy models. Given a dark energy parameter, such as the energy density Omega_Lambda or equation of state w, we split it into two meta-parameters with one controlling geometrical distances, and the other controlling the growth of structure. Observational data spanning Type Ia Supernovae, the cosmic microwave background (CMB), galaxy clustering, and weak gravitational lensing statistics are fit without requiring the two meta-parameters to be equal. This technique checks for inconsistency between different data sets, as well as for internal inconsistency within any one data set (e.g., CMB or lensing statistics) that is sensitive to both geometry and growth. We find that the cosmological constant model is consistent with current data. Theories of modified gravity generally predict a relation between growth and geometry that is different from that of general relativity. Parameter-splitting can be viewed as a crude way to parametrize the space of such theories. Our analysis of current data already appears to put sharp limits on these theories: assuming a flat universe, current data constrain the difference Omega_Lambda(geom) - Omega_Lambda(grow) to be -0.0044 +/- 0.0058 (68% C.L.); allowing the equation of state w to vary, the difference w(geom) - w(grow) is constrained to be 0.37 +/- 0.37 (68% C.L.). Interestingly, the region w(grow) > w(geom), which should be generically favored by theories that slow structure formation relative to general relativity, is quite restricted by data already. We find w(grow) < -0.80 at 2 sigma. As an example, the best-fit flat Dvali-Gabadadze-Porrati (DGP) model approximated by our parametrization lies beyond the 3 sigma contour for constraints from all the data sets."}],"oa_version":"Preprint","type":"journal_article","external_id":{"arxiv":["0705.0165"]},"date_published":"2007-09-12T00:00:00Z","citation":{"ieee":"S. Wang, L. Hui, M. May, and Z. Haiman, “Is modified gravity required by observations? An empirical consistency test of dark energy models,” <i>Physical Review D</i>, vol. 76, no. 6. American Physical Society, 2007.","short":"S. Wang, L. Hui, M. May, Z. Haiman, Physical Review D 76 (2007).","chicago":"Wang, Sheng, Lam Hui, Morgan May, and Zoltán Haiman. “Is Modified Gravity Required by Observations? An Empirical Consistency Test of Dark Energy Models.” <i>Physical Review D</i>. American Physical Society, 2007. <a href=\"https://doi.org/10.1103/physrevd.76.063503\">https://doi.org/10.1103/physrevd.76.063503</a>.","ista":"Wang S, Hui L, May M, Haiman Z. 2007. Is modified gravity required by observations? An empirical consistency test of dark energy models. Physical Review D. 76(6), 063503.","ama":"Wang S, Hui L, May M, Haiman Z. Is modified gravity required by observations? An empirical consistency test of dark energy models. <i>Physical Review D</i>. 2007;76(6). doi:<a href=\"https://doi.org/10.1103/physrevd.76.063503\">10.1103/physrevd.76.063503</a>","apa":"Wang, S., Hui, L., May, M., &#38; Haiman, Z. (2007). Is modified gravity required by observations? An empirical consistency test of dark energy models. <i>Physical Review D</i>. American Physical Society. <a href=\"https://doi.org/10.1103/physrevd.76.063503\">https://doi.org/10.1103/physrevd.76.063503</a>","mla":"Wang, Sheng, et al. “Is Modified Gravity Required by Observations? An Empirical Consistency Test of Dark Energy Models.” <i>Physical Review D</i>, vol. 76, no. 6, 063503, American Physical Society, 2007, doi:<a href=\"https://doi.org/10.1103/physrevd.76.063503\">10.1103/physrevd.76.063503</a>."},"status":"public","main_file_link":[{"url":"https://doi.org/10.48550/arXiv.0705.0165","open_access":"1"}],"doi":"10.1103/physrevd.76.063503"},{"date_created":"2024-09-06T10:18:16Z","_id":"17785","extern":"1","scopus_import":"1","publisher":"American Physical Society","publication_identifier":{"issn":["1550-7998","1550-2368"]},"author":[{"first_name":"Wenjuan","full_name":"Fang, Wenjuan","last_name":"Fang"},{"last_name":"Haiman","full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán"}],"article_type":"original","quality_controlled":"1","title":"Constraining dark energy by combining cluster counts and shear-shear correlations in a weak lensing survey","publication":"Physical Review D","volume":75,"day":"26","arxiv":1,"language":[{"iso":"eng"}],"year":"2007","intvolume":"        75","oa":1,"citation":{"apa":"Fang, W., &#38; Haiman, Z. (2007). Constraining dark energy by combining cluster counts and shear-shear correlations in a weak lensing survey. <i>Physical Review D</i>. American Physical Society. <a href=\"https://doi.org/10.1103/physrevd.75.043010\">https://doi.org/10.1103/physrevd.75.043010</a>","mla":"Fang, Wenjuan, and Zoltán Haiman. “Constraining Dark Energy by Combining Cluster Counts and Shear-Shear Correlations in a Weak Lensing Survey.” <i>Physical Review D</i>, vol. 75, no. 4, 043010, American Physical Society, 2007, doi:<a href=\"https://doi.org/10.1103/physrevd.75.043010\">10.1103/physrevd.75.043010</a>.","short":"W. Fang, Z. Haiman, Physical Review D 75 (2007).","ieee":"W. Fang and Z. Haiman, “Constraining dark energy by combining cluster counts and shear-shear correlations in a weak lensing survey,” <i>Physical Review D</i>, vol. 75, no. 4. American Physical Society, 2007.","chicago":"Fang, Wenjuan, and Zoltán Haiman. “Constraining Dark Energy by Combining Cluster Counts and Shear-Shear Correlations in a Weak Lensing Survey.” <i>Physical Review D</i>. American Physical Society, 2007. <a href=\"https://doi.org/10.1103/physrevd.75.043010\">https://doi.org/10.1103/physrevd.75.043010</a>.","ista":"Fang W, Haiman Z. 2007. Constraining dark energy by combining cluster counts and shear-shear correlations in a weak lensing survey. Physical Review D. 75(4), 043010.","ama":"Fang W, Haiman Z. Constraining dark energy by combining cluster counts and shear-shear correlations in a weak lensing survey. <i>Physical Review D</i>. 2007;75(4). doi:<a href=\"https://doi.org/10.1103/physrevd.75.043010\">10.1103/physrevd.75.043010</a>"},"date_published":"2007-02-26T00:00:00Z","doi":"10.1103/physrevd.75.043010","main_file_link":[{"url":" https://doi.org/10.48550/arXiv.astro-ph/0612187","open_access":"1"}],"status":"public","abstract":[{"text":"We study the potential of a large future weak-lensing survey to constrain dark energy properties by using both the number counts of detected galaxy clusters (sensitive primarily to density fluctuations on small scales) and tomographic shear-shear correlations (restricted to large scales). We use the Fisher matrix formalism, assume a flat universe and parameterize the equation of state of dark energy by w(a)=w_0+w_a(1-a), to forecast the expected statistical errors from either observable, and from their combination. We show that the covariance between these two observables is small, and argue that therefore they can be regarded as independent constraints. We find that when the number counts and the shear-shear correlations (on angular scales l < 1000) are combined, an LSST (Large Synoptic Survey Telescope)-like survey can yield statistical errors on (Omega_DE, w_0, w_a) as tight as (0.003, 0.03, 0.1). These values are a factor of 2-25 better than using either observable alone. The results are also about a factor of two better than those from combining number counts of galaxy clusters and their power spectrum.","lang":"eng"}],"month":"02","type":"journal_article","external_id":{"arxiv":["0612187"]},"oa_version":"Preprint","fulldoi":"https://doi.org/10.1103/physrevd.75.043010","date_updated":"2024-09-30T12:55:54Z","issue":"4","publication_status":"published","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","article_number":"043010","article_processing_charge":"No"},{"article_number":"123008","article_processing_charge":"No","publication_status":"published","issue":"12","fulldoi":"https://doi.org/10.1103/physrevd.70.123008","date_updated":"2024-09-30T09:50:28Z","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","abstract":[{"text":"We show that the abundance and redshift distribution (𝑑⁢𝑁/𝑑⁢𝑧) of galaxy clusters in future high-yield cluster surveys, combined with the spatial power spectrum [𝑃𝑐⁡(𝑘)] of the same clusters, can place significant constraints on the evolution of the dark energy equation of state, 𝑤=𝑤⁡(𝑎). We evaluate the expected errors on 𝑤𝑎=−𝑑⁢𝑤/𝑑⁢𝑎 and other cosmological parameters using a Fisher matrix approach, and simultaneously including cluster structure evolution parameters in our analysis. We study three different types of forthcoming surveys that will identify clusters based on their x-ray emission (such as DUO, the Dark Universe Observatory), their Sunyaev-Zel'dovich (SZ) decrement (such as SPT, the South Pole Telescope), or their weak-lensing shear (such as LSST, the Large Synoptic Survey Telescope). We find that combining the cluster abundance and power spectrum significantly enhances constraints from either method alone. We show that the weak-lensing survey can deliver a constraint as tight as 𝛥⁢𝑤𝑎∼0.1 on the evolution of the dark energy equation of state, and that the x-ray and SZ surveys each yield 𝛥⁢𝑤𝑎∼0.4 separately, or 𝛥⁢𝑤𝑎∼0.2 when these two surveys are combined. For the x-ray and SZ surveys, constraints on dark energy parameters are improved by a factor of 2 by combining the cluster data with cosmic microwave background anisotropy measurements by Planck, but degrade by a factor of 2 if the survey is required to solve simultaneously for cosmological and cluster structure evolution parameters. The constraint on 𝑤𝑎 from the weak-lensing survey is improved by ∼25% with the addition of Planck data.","lang":"eng"}],"month":"12","type":"journal_article","external_id":{"arxiv":["0406331"]},"oa_version":"Preprint","citation":{"ieee":"S. Wang, J. Khoury, Z. Haiman, and M. May, “Constraining the evolution of dark energy with a combination of galaxy cluster observables,” <i>Physical Review D</i>, vol. 70, no. 12. American Physical Society, 2004.","short":"S. Wang, J. Khoury, Z. Haiman, M. May, Physical Review D 70 (2004).","chicago":"Wang, Sheng, Justin Khoury, Zoltán Haiman, and Morgan May. “Constraining the Evolution of Dark Energy with a Combination of Galaxy Cluster Observables.” <i>Physical Review D</i>. American Physical Society, 2004. <a href=\"https://doi.org/10.1103/physrevd.70.123008\">https://doi.org/10.1103/physrevd.70.123008</a>.","ama":"Wang S, Khoury J, Haiman Z, May M. Constraining the evolution of dark energy with a combination of galaxy cluster observables. <i>Physical Review D</i>. 2004;70(12). doi:<a href=\"https://doi.org/10.1103/physrevd.70.123008\">10.1103/physrevd.70.123008</a>","ista":"Wang S, Khoury J, Haiman Z, May M. 2004. Constraining the evolution of dark energy with a combination of galaxy cluster observables. Physical Review D. 70(12), 123008.","mla":"Wang, Sheng, et al. “Constraining the Evolution of Dark Energy with a Combination of Galaxy Cluster Observables.” <i>Physical Review D</i>, vol. 70, no. 12, 123008, American Physical Society, 2004, doi:<a href=\"https://doi.org/10.1103/physrevd.70.123008\">10.1103/physrevd.70.123008</a>.","apa":"Wang, S., Khoury, J., Haiman, Z., &#38; May, M. (2004). Constraining the evolution of dark energy with a combination of galaxy cluster observables. <i>Physical Review D</i>. American Physical Society. <a href=\"https://doi.org/10.1103/physrevd.70.123008\">https://doi.org/10.1103/physrevd.70.123008</a>"},"date_published":"2004-12-17T00:00:00Z","doi":"10.1103/physrevd.70.123008","status":"public","main_file_link":[{"open_access":"1","url":" https://doi.org/10.48550/arXiv.astro-ph/0406331"}],"language":[{"iso":"eng"}],"year":"2004","intvolume":"        70","oa":1,"publication":"Physical Review D","volume":70,"day":"17","arxiv":1,"scopus_import":"1","publication_identifier":{"issn":["1550-7998","1550-2368"]},"publisher":"American Physical Society","article_type":"original","author":[{"last_name":"Wang","full_name":"Wang, Sheng","first_name":"Sheng"},{"first_name":"Justin","full_name":"Khoury, Justin","last_name":"Khoury"},{"first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman","full_name":"Haiman, Zoltán"},{"first_name":"Morgan","full_name":"May, Morgan","last_name":"May"}],"title":"Constraining the evolution of dark energy with a combination of galaxy cluster observables","quality_controlled":"1","extern":"1","date_created":"2024-09-06T10:00:53Z","_id":"17770"}]