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typical Feynman diagrams for the $\\alpha_{s}^{4}$ QCD part of $gg\\toc\\bar{c}[^3S_1,\\underline{1}]+c+\\bar{c}$.","source":"arxiv","key":"6f1efd2c2196bf7996b068dff53953fa","url":"https://inspirehep.net/files/6f1efd2c2196bf7996b068dff53953fa"},{"filename":"diagQED1.png","caption":"The typical Type I Feynman diagrams in the LO ($\\alpha^{2}\\alpha_{s}^2$) QED part of $gg\\to c\\bar{c}[^3S_1,\\underline{1}]+c+\\bar{c}$.","source":"arxiv","key":"b645684408356d3ed243f3c6222c4cf7","url":"https://inspirehep.net/files/b645684408356d3ed243f3c6222c4cf7"},{"filename":"diagQED2.png","caption":"The typical Type II Feynman diagrams of photon fragmentation in the LO ($\\alpha^{2}\\alpha_{s}^2$) QED part of $gg\\to c\\bar{c}[^3S_1,\\underline{1}]+c+\\bar{c}$.","source":"arxiv","key":"86a6b808496587395d0fd352d73551e9","url":"https://inspirehep.net/files/86a6b808496587395d0fd352d73551e9"},{"filename":"diagqqb.png","caption":"The typical Feynman diagrams of the LO process of $q\\bar{q}\\to c\\bar{c}[^3S_1,\\underline{1}]+c+\\bar{c}$ for QCD and QED.","source":"arxiv","key":"677d8a742e32d0480f4e2e58c8254c46","url":"https://inspirehep.net/files/677d8a742e32d0480f4e2e58c8254c46"},{"filename":"qedqcdpt.png","caption":"(a): The $p_t$ distributions of the production rate for $J/\\psi + c + \\bar{c}$ hadroproduction at the Tevatron ($\\sqrt{s}=$1.96TeV, $|y|<$0.6, 3GeV$<$pt$<$50GeV) and LHC ($\\sqrt{s}=$14TeV, $|y|<$3, 3GeV$<$pt$<$100GeV). (b): the $p_t$ distributions of the ``total\" with $\\mu_r=\\mu_f=\\mu$ dependence. Where the total refers to the sum of the QCD, QED and their interference results.","source":"arxiv","key":"85e58b04e099419de2ff93a081bd14e9","url":"https://inspirehep.net/files/85e58b04e099419de2ff93a081bd14e9"},{"filename":"qcedpt.png","caption":"(a): The $p_t$ distributions of the production rate for $J/\\psi + c + \\bar{c}$ hadroproduction at the Tevatron ($\\sqrt{s}=$1.96TeV, $|y|<$0.6, 3GeV$<$pt$<$50GeV) and LHC ($\\sqrt{s}=$14TeV, $|y|<$3, 3GeV$<$pt$<$100GeV). (b): the $p_t$ distributions of the ``total\" with $\\mu_r=\\mu_f=\\mu$ dependence. Where the total refers to the sum of the QCD, QED and their interference results.","source":"arxiv","key":"504668aaafc098257f4c8ae5d0871ff6","url":"https://inspirehep.net/files/504668aaafc098257f4c8ae5d0871ff6"},{"filename":"tevptl.png","caption":"The $p_t$ distribution of polarization parameter $\\alpha$ for the $J/\\psi + c + \\bar{c}$ hadroproduction at the Tevatron (a) and LHC (b). Here, the total refersto the sum of the QCD, QED and their interference results.","source":"arxiv","key":"824536c3292629efb6961975e406896b","url":"https://inspirehep.net/files/824536c3292629efb6961975e406896b"},{"filename":"lhcptl.png","caption":"The $p_t$ distribution of polarization parameter $\\alpha$ for the $J/\\psi + c + \\bar{c}$ hadroproduction at the Tevatron (a) and LHC (b). Here, the total refersto the sum of the QCD, QED and their interference results.","source":"arxiv","key":"12a41f8f0fab73f55137c6be8bdcd4f4","url":"https://inspirehep.net/files/12a41f8f0fab73f55137c6be8bdcd4f4"}],"legacy_version":"20160326143950.0","inspire_categories":[{"term":"Phenomenology-HEP"}],"first_author":{"affiliations_identifiers":[{"schema":"ROR","value":"https://ror.org/03v8tnc06"}],"full_name":"He, Zhi-Guo","last_name":"He","ids":[{"schema":"ORCID","value":"0000-0001-9887-2058"}],"first_name":"Zhi-Guo","recid":1057092},"control_number":817900,"dois":[{"value":"10.1103/PhysRevD.79.094003"}],"document_type":["article"],"texkeys":["He:2009zzb"],"abstracts":[{"source":"arXiv","value":"We calculate \\alpha^{2}\\alpha_{s}^{2} order QED contribution to J/\\psi production in pp(\\bar{p})\\to J/\\psi+c\\bar{c} color-singlet process at the Tevatron and LHC in the framework of non-relativistic QCD. The contribution of the interference between the \\alpha^{2}\\alpha_{s}^{2} QED and \\alpha_{s}^{4} QCD is also taken into account. The J/\\psi production associated with a charm quark pair could be a measurable signal at hadron collider experiment. Our calculations show that by including the QED contribution, the p_{t} distribution is enhanced by a factor of 1.5 (1.9) at the Tevatron (LHC) at p_{t}=50 (100) GeV. In addition, the polarization of J/\\psi turns from unpolarized in all region to increasingly transverse when p_{t} becomes larger.","abstract_source_suggest":{"input":"arXiv"}}],"primary_arxiv_category":["hep-ph"],"titles":[{"title":"QED contribution to the production of J/psi + c anti-c + X at the Tevatron and LHC"},{"source":"arXiv","title":"QED contribution to the production of J/\\psi+c\\bar{c}+X at the Tevatron and LHC"}],"curated":true},"links":{"bibtex":"https://inspirehep.net/api/literature/817900?format=bibtex","latex-eu":"https://inspirehep.net/api/literature/817900?format=latex-eu","latex-us":"https://inspirehep.net/api/literature/817900?format=latex-us","json":"https://inspirehep.net/api/literature/817900?format=json","json-expanded":"https://inspirehep.net/api/literature/817900?format=json-expanded","cv":"https://inspirehep.net/api/literature/817900?format=cv","citations":"https://inspirehep.net/api/literature/?q=refersto%3Arecid%3A817900"},"updated":"2023-03-10T00:34:39.220197+00:00","created":"2009-04-14T00:00:00+00:00","id":"817900"},{"metadata":{"publication_info":[{"year":2024}],"citation_count":0,"authors":[{"full_name_unicode_normalized":"noordhuis, d.","full_name":"Noordhuis, D.","record":{"$ref":"https://inspirehep.net/api/authors/1975833"},"last_name":"Noordhuis","ids":[{"schema":"INSPIRE BAI","value":"D.Noordhuis.1"}],"first_name":"D.","uuid":"051a2648-54ef-4dcc-9611-5614b1017504","recid":1975833}],"citation_count_without_self_citations":0,"isbns":[{"value":"9789493391352"}],"$schema":"https://inspirehep.net/schemas/records/hep.json","number_of_pages":215,"inspire_categories":[{"term":"Astrophysics","source":"curator"}],"author_count":1,"urls":[{"value":"https://dare.uva.nl/search?identifier=84158e2d-eb8f-40df-bf0a-632fb04a35df"}],"first_author":{"full_name":"Noordhuis, D.","last_name":"Noordhuis","first_name":"D.","recid":1975833},"control_number":2831395,"earliest_date":"2024","document_type":["thesis"],"texkeys":["Noordhuis:2024goa"],"abstracts":[{"source":"Amsterdam U.","value":"This thesis explores the potential of neutron stars as laboratories for studying axions, a hypothetical particle widely regardedas a leading candidate for dark matter. The research centers on two key mechanisms occurring within the region surroundingneutron stars, known as the magnetosphere: resonant axion-photon mixing and axion production via vacuum gaps. The former refersto the conversion of axions into photons, and vice versa, at locations where their four-momenta align; the latter refers tothe generation of axions in specific regions of the magnetosphere, where this process is facilitated by the presence of oscillatingelectromagnetic fields. The thesis first presents a framework for calculating the photon flux produced by the resonant mixing of dark matter axionsin neutron star magnetospheres, accounting for the complex nature of the magnetospheric plasma. The resulting signals aremore complex than previously anticipated, being characterized by strong anisotropy and time dependence. Next, the thesis examinesaxions produced locally within neutron star vacuum gaps. It is shown that the relativistic part of this local axion populationproduces a broadband radio flux through resonant mixing. By comparing these results to observations of nearby pulsars, strongobservational constraints on the axion-photon coupling are established. The non-relativistic part of the population insteadleads to the formation of an axion cloud around the parent neutron star, a phenomenon studied here for the first time. Itis demonstrated that axion clouds have the potential to reach enormous densities and furthermore generate observable effectsthrough resonant mixing. 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The solid line is the least square fit to the points (Eq.(\\ref{eqEWfit})), and the dashed line refersto the one-to-one relation.","source":"arxiv","key":"9e12d9df89144a72a14f1a82197323dc","url":"https://inspirehep.net/files/9e12d9df89144a72a14f1a82197323dc"},{"filename":"fig3.png","caption":"The abundance patterns of sample stars.","source":"arxiv","key":"fd43884850eb5290d025d4cbeeee10a3","url":"https://inspirehep.net/files/fd43884850eb5290d025d4cbeeee10a3"},{"filename":"fig4a.png","caption":"To check the reliability of the determined atmospheric parameters $\\teff$/log$g$/$\\xi_t$ of the stars by taking HD216219 as an example: (a). Fe abundances from Fe\\,I lines as a function of excitation potential. There is no significant trend of [Fe/H] with $\\chi$, indicating a correct temperature distribution in the model atmosphere. (b). The consistence of the Fe\\,I and Fe,II abundances (the filled and open circles refer to the Fe\\,I and Fe\\,II abundances respectively), which mean that the determined log$g$ are reliable; and an illustration of the determination of the microturbulence velocity since there is no significant trendbetween [Fe/H] and EWs.","source":"arxiv","key":"0aae66627c42f72211e1a9b4c2adc1ce","url":"https://inspirehep.net/files/0aae66627c42f72211e1a9b4c2adc1ce"},{"filename":"fig4b.png","caption":"To check the reliability of the determined atmospheric parameters $\\teff$/log$g$/$\\xi_t$ of the stars by taking HD216219 as an example: (a). Fe abundances from Fe\\,I lines as a function of excitation potential. There is no significant trend of [Fe/H] with $\\chi$, indicating a correct temperature distribution in the model atmosphere. (b). The consistence of the Fe\\,I and Fe,II abundances (the filled and open circles refer to the Fe\\,I and Fe\\,II abundances respectively), which mean that the determined log$g$ are reliable; and an illustration of the determination of the microturbulence velocity since there is no significant trendbetween [Fe/H] and EWs.","source":"arxiv","key":"132ddf4c82ec18e856914eac24ffd299","url":"https://inspirehep.net/files/132ddf4c82ec18e856914eac24ffd299"},{"filename":"fig5a.png","caption":"The comparisons between our abundances determinations and those of Smith et al. (1993) for the two common stars: (a). for HD\\,4395; (b). for HD\\,216219. The solid lines are the least square fits for the data and the dashed lines are the one-to-one relations. 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The vertical bar indicates the gas massfraction.","source":"arxiv","key":"9916e09b2d34328c3fbb0f0bdf0c37ec","url":"https://inspirehep.net/files/9916e09b2d34328c3fbb0f0bdf0c37ec"},{"filename":"WW_zt.png","caption":"Gas (IGM) metallicity-density relation (without explicitly splitting the star-forming particles in the hot and the cold phases), for the WW (Weak galactic Winds of 100 km/s; left panel), SW (Strong galactic Winds of 600 km/s; middle panel) and MDW (Momentum-Driven galactic Winds; right panel) simulations at $z=3$.The vertical bar indicates the gas mass fraction.","source":"arxiv","key":"22f70cccc8f00d60965b4c2e1af5b9e3","url":"https://inspirehep.net/files/22f70cccc8f00d60965b4c2e1af5b9e3"},{"filename":"SW_zt.png","caption":"Gas (IGM) metallicity-density relation (without explicitly splitting the star-forming particles in the hot and the cold phases), for the WW (Weak galactic Winds of 100 km/s; left panel), SW (Strong galactic Winds of 600 km/s; middle panel) and MDW (Momentum-Driven galactic Winds; right panel) simulations at $z=3$.The vertical bar indicates the gas mass fraction.","source":"arxiv","key":"dee6962d22e3bb3ea8fc65800a72b592","url":"https://inspirehep.net/files/dee6962d22e3bb3ea8fc65800a72b592"},{"filename":"MDW_zt.png","caption":"Gas (IGM) metallicity-density relation (without explicitly splitting the star-forming particles in the hot and the cold phases), for the WW (Weak galactic Winds of 100 km/s; left panel), SW (Strong galactic Winds of 600 km/s; middle panel) and MDW (Momentum-Driven galactic Winds; right panel) simulations at $z=3$.The vertical bar indicates the gas mass fraction.","source":"arxiv","key":"67a59a295c7c578f488bc28749ad09c8","url":"https://inspirehep.net/files/67a59a295c7c578f488bc28749ad09c8"},{"filename":"sfr_rv.png","caption":"{\\it {Left Panel}}: cosmic star formation rate (SFR) for some of the hydrodynamical simulations of Table I. {\\it Right Panel}: evolution of the total $\\Omega_{\\rm HI}$ ($\\times 1000$) as a function of redshift for some of the hydrodynamicalsimulations of Table I.","source":"arxiv","key":"ea0c740e29534e8023b96cda3865fd96","url":"https://inspirehep.net/files/ea0c740e29534e8023b96cda3865fd96"},{"filename":"OmegaHI_MDW_rv.png","caption":"{\\it {Left Panel}}: cosmic star formation rate (SFR) for some of the hydrodynamical simulations of Table I. {\\it Right Panel}: evolution of the total $\\Omega_{\\rm HI}$ ($\\times 1000$) as a function of redshift for some of the hydrodynamicalsimulations of Table I.","source":"arxiv","key":"5b4c54ab4e930476fbebe035921d8ad4","url":"https://inspirehep.net/files/5b4c54ab4e930476fbebe035921d8ad4"},{"filename":"OmegaC4_PAPER.png","caption":"Evolution of the total $\\Omega_{\\rm CIV}$ (upper panels) and the total $\\Omega_{\\rm OVI}$ (lower panels) as a function of redshift for some of the hydrodynamical simulations of Table I. {\\it {Left Panels}}: effect of different wind strengths and implementations. {\\it {Middle Panels}}: effect of differentIMFs. {\\it {Right Panels}}: resolution tests.","source":"arxiv","key":"13fa791fddf85bd3ea5b98dd91fdef3b","url":"https://inspirehep.net/files/13fa791fddf85bd3ea5b98dd91fdef3b"},{"filename":"OmegaO6_PAPER.png","caption":"Evolution of the total $\\Omega_{\\rm CIV}$ (upper panels) and the total $\\Omega_{\\rm OVI}$ (lower panels) as a function of redshift for some of the hydrodynamical simulations of Table I. {\\it {Left Panels}}: effect of different wind strengths and implementations. {\\it {Middle Panels}}: effect of differentIMFs. {\\it {Right Panels}}: resolution tests.","source":"arxiv","key":"58e08c8d6f81b44b6230b7e67ff79ef4","url":"https://inspirehep.net/files/58e08c8d6f81b44b6230b7e67ff79ef4"},{"filename":"dndMPAPER.png","caption":"Differential halo mass function (number of haloes of a given mass per unit mass [$h^{-1}M_{\\rm \\odot}$] and per unit volume [Mpc$^3$/$h^3$]) for runs SW, SW$_{\\rm 5,320}$, SW$_{\\rm 20,512}$ atredshift $z=3$, compared with \\citet{shethtormen99} prediction.","source":"arxiv","key":"8046daa94b252b3f74c68e2498477e63","url":"https://inspirehep.net/files/8046daa94b252b3f74c68e2498477e63"},{"filename":"dla_256_WW.png","caption":"HI column density maps in a slice around the same massive halo in the WW (upper panel), SW (middle panel) and MDW (lowerpanel) runs at $z=3$.","source":"arxiv","key":"04739d6541ae043a736e34092feeed75","url":"https://inspirehep.net/files/04739d6541ae043a736e34092feeed75"},{"filename":"dla_256_SW.png","caption":"HI column density maps in a slice around the same massive halo in the WW (upper panel), SW (middle panel) and MDW (lowerpanel) runs at $z=3$.","source":"arxiv","key":"e22614869ca0d288f6129ee053f0a17f","url":"https://inspirehep.net/files/e22614869ca0d288f6129ee053f0a17f"},{"filename":"dla_256_MDW.png","caption":"HI column density maps in a slice around the same massive halo in the WW (upper panel), SW (middle panel) and MDW (lowerpanel) runs at $z=3$.","source":"arxiv","key":"03a05de124da9a60a631aecd643a7cb7","url":"https://inspirehep.net/files/03a05de124da9a60a631aecd643a7cb7"},{"filename":"sfr_group_3in1_MDW_tex.png","caption":"Star formation rates (in $M_{\\rm \\odot}$ per year) plotted asa function of halo mass for SW, WW and MDW runs at $z=3$.","source":"arxiv","key":"7d102b851614b83c1d3991cc186b8dac","url":"https://inspirehep.net/files/7d102b851614b83c1d3991cc186b8dac"},{"filename":"met_group_3in1_MDW_tex.png","caption":"Mean total metallicity in solar unit plotted as a functionof halo mass for SW, WW and MDW runs at $z=3$.","source":"arxiv","key":"ffde1a87110a1026531d885dbc785ff4","url":"https://inspirehep.net/files/ffde1a87110a1026531d885dbc785ff4"},{"filename":"nhi_group_3in1_MDW_new.png","caption":"Mean neutral fraction of hydrogen (HI/H) plotted as afunction of halo mass for SW, WW and MDW runs at $z=3$.","source":"arxiv","key":"ec28df4be5afbd3edf6847f91cfe3d6f","url":"https://inspirehep.net/files/ec28df4be5afbd3edf6847f91cfe3d6f"},{"filename":"crossfit3in1_MDW_rv.png","caption":"Triangles represent the DLA cross-sections (in comoving units) as a function of the total halo mass for the SW run at $z=2.25,3,4$. The overplotted lines show power-law fits, of the form $\\log \\sigma_{\\rm DLA}= \\alpha (\\log M_{\\rm tot} - 12) + \\beta$, to the data points for the SW itself (dashed black line), WW (dot-dashed blue line) and MDW (triple-dot-dashed cyan line) runs. The continuous red lines in the middle panel fit the upper andlower envelopes of the SW distribution at $z=3$.","source":"arxiv","key":"3c2f55ef9f9c440b0ef523208bfa33cb","url":"https://inspirehep.net/files/3c2f55ef9f9c440b0ef523208bfa33cb"},{"filename":"DLAcum3in1_MDW_32_rv.png","caption":"Cumulative abundance of DLAs per unit redshift as a function of total halo mass for the SW (dashed black line), WW (dot-dashed blue line) and MDW (triple-dot-dashed cyan line) runs at redshift $z=3$. The continuous red lines show the results considering the scatter (in a conservative way) in the cross-section vs mass relation for the SW run. The red shaded region indicates the observed cumulative DLA abundance of \\citet{prochaska05} from SDSSdata.","source":"arxiv","key":"782e69ce49a4ad0d738210e07147848e","url":"https://inspirehep.net/files/782e69ce49a4ad0d738210e07147848e"},{"filename":"cdensdistr3in1_MDW.png","caption":"{\\it Left Panel}: HI column density distribution function at $z=3$ for the SW (dashed black line), WW (dot-dashed blue line), SW$_{\\rm 20,512}$ (dotted red line) and MDW (triple-dot-dashed cyan line) runs. {\\it Right Panel}: Contribution to the HI column density distribution function from haloes of different mass in the SW$_{\\rm 20,512}$ run at $z=3$. Cyan triple dot-dashed line refers to haloes with mass in the range 10$^9-10^{10}h^{-1}M_{\\rm \\odot}$, orange dot-dashed line refers to haloes with mass in the range 10$^{10}-10^{11}h^{-1}M_{\\rm \\odot}$, red dotted line refers to haloes with mass greater than 10$^{11}h^{-1}M_{\\rm \\odot}$ while black dashed line refers to all haloes. In both the panels the overplotted black diamonds and the solid line show the data pointsand the fit of \\citet{prochaska05}.","source":"arxiv","key":"917d9a7b4d5e3ee43bba0b396017b9f5","url":"https://inspirehep.net/files/917d9a7b4d5e3ee43bba0b396017b9f5"},{"filename":"cdensdistr4000div.png","caption":"{\\it Left Panel}: HI column density distribution function at $z=3$ for the SW (dashed black line), WW (dot-dashed blue line), SW$_{\\rm 20,512}$ (dotted red line) and MDW (triple-dot-dashed cyan line) runs. {\\it Right Panel}: Contribution to the HI column density distribution function from haloes of different mass in the SW$_{\\rm 20,512}$ run at $z=3$. Cyan triple dot-dashed line refers to haloes with mass in the range 10$^9-10^{10}h^{-1}M_{\\rm \\odot}$, orange dot-dashed line refers to haloes with mass in the range 10$^{10}-10^{11}h^{-1}M_{\\rm \\odot}$, red dotted line refers to haloes with mass greater than 10$^{11}h^{-1}M_{\\rm \\odot}$ while black dashed line refers to all haloes. In both the panels the overplotted black diamonds and the solid line show the data pointsand the fit of \\citet{prochaska05}.","source":"arxiv","key":"61e2bed5873c0d799b20cfcb4f1b26be","url":"https://inspirehep.net/files/61e2bed5873c0d799b20cfcb4f1b26be"},{"filename":"cdensdistr3in1_MDWz2.png","caption":"{\\it Left Panel}: HI column density distribution function at $z=2.25$ for the SW (dashed black line), WW (dot-dashed blue line) and MDW (triple-dot-dashed cyan line) runs. Overplotted black diamonds and solid line show the data points and the fit of \\citet{prochaska05}. Run SW$_{\\rm 20,512}$ is not present here because this simulation was stopped at $z=3$. {\\it Right Panel}: the same as the left panel but at redshift $z=4$. Dotted red line refersto the SW$_{\\rm 20,512}$ run.","source":"arxiv","key":"359da61be416ef0e98fb7b5c4d3cfdc1","url":"https://inspirehep.net/files/359da61be416ef0e98fb7b5c4d3cfdc1"},{"filename":"cdensdistr3in1_MDWz4.png","caption":"{\\it Left Panel}: HI column density distribution function at $z=2.25$ for the SW (dashed black line), WW (dot-dashed blue line) and MDW (triple-dot-dashed cyan line) runs. Overplotted black diamonds and solid line show the data points and the fit of \\citet{prochaska05}. Run SW$_{\\rm 20,512}$ is not present here because this simulation was stopped at $z=3$. {\\it Right Panel}: the same as the left panel but at redshift $z=4$. Dotted red line refersto the SW$_{\\rm 20,512}$ run.","source":"arxiv","key":"96deb8fb38a2d22f2f56492314dc2d91","url":"https://inspirehep.net/files/96deb8fb38a2d22f2f56492314dc2d91"},{"filename":"OmegaDLA.png","caption":"Redshift evolution of $\\Omega_{\\rm DLA}$ for the SW (black solid line), WW (blue dotted line) and MDW (cyan triple-dot-dashed line) runs. Overplotted are the result of \\citet{pontzen08} (green cross) and the observational estimate of \\citet{prochaska05} (reddiamonds) and \\citet{peroux05} (orange triangles).","source":"arxiv","key":"10e13d31880f5890bf8bcbfd62c372f2","url":"https://inspirehep.net/files/10e13d31880f5890bf8bcbfd62c372f2"},{"filename":"spectra_overlap3in1_MDW.png","caption":"Comparison of physical quantities extracted from three simulated LOSs passing through the center of mass of the second most massive halo for the SW (solid black line), WW (dashed blue line) and MDW (dotted red line) runs at $z=3$. From top to bottom the figure shows: total gas density [n$_{\\rm H}/$cm$^{3}$], HI density [n$_{\\rm H}/$cm$^{3}$], total metallicity (in solar unit),temperature [K] and peculiar velocity field [km/s].","source":"arxiv","key":"164be1c4fd8e9cf745769e35df12624b","url":"https://inspirehep.net/files/164be1c4fd8e9cf745769e35df12624b"},{"filename":"veldistr_selfshield.png","caption":"{\\it Left Panel}: DLAs velocity width distribution in runs SW$_{\\rm 20,512}$ (dotted red line), WW (dot-dashed blue line), MDW (triple-dot-dashed cyan line) and SW$_{\\rm 20,512}$ $smoothed$ (solid black line) at $z=3$. {\\it Right Panel}: DLAs velocity width distribution in runs SW$_{\\rm 20,512}\\_\\tau_{\\rm HI}$ (solid red line), WW$\\_\\tau_{\\rm HI}$ (solid blue line), MDW$\\_\\tau_{\\rm HI}$ (solid cyan line) and SW$_{\\rm 20,512}$ $smoothed$ (solid black line) at $z=3$. In both the panels the overplotted black diamondsshow the observational data of \\citet{prochaska08}.","source":"arxiv","key":"11ebfac02b39e783b6f094dba8e32874","url":"https://inspirehep.net/files/11ebfac02b39e783b6f094dba8e32874"},{"filename":"veldistr_Pontzen.png","caption":"{\\it Left Panel}: DLAs velocity width distribution in runs SW$_{\\rm 20,512}$ (dotted red line), WW (dot-dashed blue line), MDW (triple-dot-dashed cyan line) and SW$_{\\rm 20,512}$ $smoothed$ (solid black line) at $z=3$. {\\it Right Panel}: DLAs velocity width distribution in runs SW$_{\\rm 20,512}\\_\\tau_{\\rm HI}$ (solid red line), WW$\\_\\tau_{\\rm HI}$ (solid blue line), MDW$\\_\\tau_{\\rm HI}$ (solid cyan line) and SW$_{\\rm 20,512}$ $smoothed$ (solid black line) at $z=3$. In both the panels the overplotted black diamondsshow the observational data of \\citet{prochaska08}.","source":"arxiv","key":"143fdcb7a8a623b7af0180bcf53f06f7","url":"https://inspirehep.net/files/143fdcb7a8a623b7af0180bcf53f06f7"},{"filename":"PDFvm_rv.png","caption":"Contribution to the DLAs velocity width distribution from haloes of different mass in runs SW$_{\\rm 20,512}\\_\\tau_{\\rm HI}$ (solid + dashed red lines), WW$\\_\\tau_{\\rm HI}$ (solid + dashed blue lines), MDW$\\_\\tau_{\\rm HI}$ (solid + dashed cyan lines) at $z=3$. For the different runs, dashed lines refer to haloes with mass lower than $10^{10.5}h^{-1}M_{\\rm \\odot}$ and solid lines refers to haloes with mass greater than $10^{10.5}h^{-1}M_{\\rm \\odot}$. The overplotted black diamonds show the observationaldata of \\citet{prochaska08}.","source":"arxiv","key":"9c0da7347387a1afe507cec83a61138c","url":"https://inspirehep.net/files/9c0da7347387a1afe507cec83a61138c"},{"filename":"met-dvel_MDW_tauh1.png","caption":"{\\it Left Panel}: relationship between metallicity and SiII velocity width of individual sightlines through haloes in MDW\\_$\\tau_{\\rm HI}$ (green solid squares) and SW$_{\\rm 20,512} smoothed$ (red solid diamonds) at $z=3$, compared to the observational data by \\citet{prochaska08} (black crosses). {\\it Right Panel}: relationship between metallicity and SiII velocity width of individual sightlines through haloes with masses $M > 10^{10.5}h^{-1}M_{\\rm \\odot}$ (red solid diamonds), $M > 10^{10}h^{-1}M_{\\rm \\odot}$ (green solid squares) and $M > 10^{9.5}h^{-1}M_{\\rm \\odot}$ (blue solid triangles) in MDW\\_$\\tau_{\\rm HI}$ run at $z=3$, compared to the observational data by \\citet{prochaska08}(black crosses).","source":"arxiv","key":"ec634ff4defc3a5399aa2da6f6624032","url":"https://inspirehep.net/files/ec634ff4defc3a5399aa2da6f6624032"},{"filename":"met-dvel_MDW_tauh1_hdev.png","caption":"{\\it Left Panel}: relationship between metallicity and SiII velocity width of individual sightlines through haloes in MDW\\_$\\tau_{\\rm HI}$ (green solid squares) and SW$_{\\rm 20,512} smoothed$ (red solid diamonds) at $z=3$, compared to the observational data by \\citet{prochaska08} (black crosses). {\\it Right Panel}: relationship between metallicity and SiII velocity width of individual sightlines through haloes with masses $M > 10^{10.5}h^{-1}M_{\\rm \\odot}$ (red solid diamonds), $M > 10^{10}h^{-1}M_{\\rm \\odot}$ (green solid squares) and $M > 10^{9.5}h^{-1}M_{\\rm \\odot}$ (blue solid triangles) in MDW\\_$\\tau_{\\rm HI}$ run at $z=3$, compared to the observational data by \\citet{prochaska08}(black crosses).","source":"arxiv","key":"1dc921aa537d287a3fdc88ae91baa617","url":"https://inspirehep.net/files/1dc921aa537d287a3fdc88ae91baa617"}],"legacy_version":"20170220222820.0","inspire_categories":[{"term":"Astrophysics"}],"first_author":{"full_name":"Tescari, Edoardo","last_name":"Tescari","first_name":"Edoardo","recid":2330529},"control_number":818557,"dois":[{"source":"ADS","value":"10.1111/j.1365-2966.2009.14943.x"}],"document_type":["article"],"texkeys":["Tescari:2009mj"],"abstracts":[{"source":"arXiv","value":"We investigate the properties of Damped Lyman-alpha systems (DLAs) using high-resolution and large box-size cosmological hydrodynamical simulations of a LambdaCDM model. The numerical code used is a modification of GADGET-2 with a self consistent implementation of the metal enrichment mechanism (Tornatore et al. 2007). We explore the numerical convergence of some relevant physical quantities and we vary the parameters describing the properties of galactic winds; the initial stellar mass function; the linear dark matter power spectrum and the metal enrichment pattern of the IGM (Intergalactic Medium) around DLAs. We find that strong galactic winds with speed of about 600 km/s, in an energy-driven wind scenario, are needed in order to match the observed column density distribution function for DLAs and the evolution of the neutral hydrogen content with redshift. The momentum-driven implementation of the galactic wind model, that relates the speed and mass load in the wind to the properties of the dark matter haloes, shows a behaviour which is intermediate between the energy-driven galactic winds of small (100 km/s) and large (600 km/s) velocities. At z=3 the contribution of haloes of masses between 10^9 and 10^10 h^-1 M_sun, for DLAs below 10^20.8 cm^-2, to the column density distribution function, is significant. By interpolating physical quantities along line-of-sights through massive haloes we qualitatively show how different galactic wind models impact on the IGM around DLAs. Furthermore, we analyse statistics related to the velocity widths of SiII associated to DLAs: the metallicity in the wind seems to be rather clumpy and this produces an underestimation of the observed velocity widths. We outline possible solutions to this problem.","abstract_source_suggest":{"input":"arXiv"}}],"primary_arxiv_category":["astro-ph.CO"],"titles":[{"title":"Damped Lyman-alpha systems in high-resolution hydrodynamical simulations"},{"source":"arXiv","title":"Damped Lyman-alpha systems in high-resolution hydrodynamical simulations"}],"curated":false},"links":{"bibtex":"https://inspirehep.net/api/literature/818557?format=bibtex","latex-eu":"https://inspirehep.net/api/literature/818557?format=latex-eu","latex-us":"https://inspirehep.net/api/literature/818557?format=latex-us","json":"https://inspirehep.net/api/literature/818557?format=json","json-expanded":"https://inspirehep.net/api/literature/818557?format=json-expanded","cv":"https://inspirehep.net/api/literature/818557?format=cv","citations":"https://inspirehep.net/api/literature/?q=refersto%3Arecid%3A818557"},"updated":"2023-03-06T22:43:57.428075+00:00","created":"2009-04-23T00:00:00+00:00","id":"818557"},{"metadata":{"citation_count":0,"authors":[{"full_name_unicode_normalized":"gordienko, alexey","full_name":"Gordienko, Alexey","record":{"$ref":"https://inspirehep.net/api/authors/1971301"},"last_name":"Gordienko","ids":[{"schema":"INSPIRE BAI","value":"A.Gordienko.1"}],"signature_block":"GARDANCa","uuid":"501540de-88af-4ba5-9042-bdca2bfa2a4a","first_name":"Alexey","recid":1971301}],"citation_count_without_self_citations":0,"citeable":true,"$schema":"https://inspirehep.net/schemas/records/hep.json","references":[{"reference":{"texkey":"ArnoldBook","label":"1","publication_info":{"year":2003},"misc":["методы классической механики. М.: Эдиториал УРСС,, 416 с"],"authors":[{"full_name":"Математические, Арнольд В.И."}]},"raw_refs":[{"schema":"text","source":"arXiv","value":"[1] Арнольд В. И. Математические методы классической механики. М.: Эдиториал УРСС, 2003, 416 с."}]},{"reference":{"texkey":"AtiyahMacdonald","label":"2","publication_info":{"year":1972},"misc":["в коммутативную алгебру. М.: Мир,, 160 с"],"authors":[{"full_name":"М., Атья"},{"full_name":"Ввведение, Макдональд И."}]},"raw_refs":[{"schema":"text","source":"arXiv","value":"[2] Атья М., Макдональд И. Ввведение в коммутативную алгебру. М.: Мир, 1972, 160 с."}]},{"reference":{"texkey":"Bahturin","label":"3","publication_info":{"year":1985},"misc":["в алгебрах Ли. М.: Наука,, 448 c"],"authors":[{"full_name":"Тождества, Бахтурин Ю.А."}]},"raw_refs":[{"schema":"text","source":"arXiv","value":"[3] Бахтурин Ю. А. Тождества в алгебрах Ли. М.: Наука, 1985, 448 c."}]},{"reference":{"texkey":"BahturinZaicevSegal","label":"4","publication_info":{"year":2008},"misc":["простые градуированные алгебры. Матем. сб., 199:7 , 21-40"],"authors":[{"full_name":"А., Бахтурин Ю."},{"full_name":"В., Зайцев М."},{"full_name":"Конечномерные, Сегал С.К."}]},"raw_refs":[{"schema":"text","source":"arXiv","value":"[4] Бахтурин Ю. А., Зайцев М. В., Сегал С. К. Конечномерные простые градуированные алгебры. Матем. сб., 199:7 (2008), 21–40."}]},{"reference":{"texkey":"VerZaiMishch","label":"5","publication_info":{"year":2011},"misc":["условие совпадения нижней и верхней экспонент многообразия линейных алгебр. Вестн. Моск. ун-та. Сер. 1. Матем., мех., №2 , 36-39"],"authors":[{"full_name":"Б., Верёвкин А."},{"full_name":"В., Зайцев М."},{"full_name":"Достаточное, Мищенко С.П."}]},"raw_refs":[{"schema":"text","source":"arXiv","value":"[5] Верёвкин А. Б., Зайцев М. В., Мищенко С. П. 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shower matching and merging\n\nMarek Schönherr∗†\nTheoretical Physics Department, CERN, Geneva, Switzerland\nE-mail: marek.schoenherr@cern.ch\n\nWith Run-II of the LHC starting its final year of data-taking, high precision theoretical predictions\nthrough Monte-Carlo event generators whose uncertainties match that of the recorded data are of\nhighest importance. This talk summarises the progress of the field and highlight a number of\nrecent developments.\n\nCorfu Summer Institute 2017 ’School and Workshops on Elementary Particle Physics and Gravity’\n2-28 September 2017\nCorfu, Greece\n\n∗Speaker.\n†M.S. was supported by PITN–GA–2012–315877 (MCnet) and the ERC Advanced Grant MC@NNLO (340983).\n\nc© Copyright owned by the author(s) under the terms of the Creative Commons\nAttribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). https://pos.sissa.it/\n\nmailto:marek.schoenherr@cern.ch\n\n\nP\no\nS\n(\nC\nO\nR\nF\nU\n2\n0\n1\n7\n)\n1\n1\n0\n\nParton shower matching and merging Marek Schönherr\n\n1. Introduction\n\nModern Monte-Carlo event generators like PYTHIA [1], HERWIG [2, 3] or SHERPA [4, 5, 6,\n7, 8, 9, 10, 11] are the workhorses for the physics analyses and measurements at the LHC. In\nmany cases, the PYTHIA and HERWIG generators (or their older predecessors) receive input from\nparton level tools which compute the hard core production matrix elements either at LO (ALPGEN\n\n[12] or MADGRAPH5_aMC@NLO [13]), NLO (MADGRAPH5_aMC@NLO or POWHEG [14]) or\neven NNLO (POWHEG-MiNLO [15, 16, 17, 18] or GENEVA [19]), which are matched to the parton\nshower. The following contribution thus highlights a few important improvements that become\navailable in recent years, some of the forming the standard for the experiments now.\n\n2. Matching next-to-leading order matrix elements to parton showers\n\nIn a first step, the matching of NLO matrix elementsto parton showers, which is known for over\na decade now, is briefly reviewed. In the literature, there exist various different ansatzes: POWHEG\n\n[20, 21] and MC@NLO [22, 23], and various variants therof [24, 25, 26, 27, 28, 29, 30, 31]. They\nare available for all processes of interest and, thus, for the minimum baseline standard in LHC\nphysics analyses. Their general aim is to keep both the NLO accuracy in an expansion of the cross\nsection in αs at the same time as the full logarithmic accuracy of the parton shower resummation.\n\n〈O〉NLOPS =\n∫\n\ndΦB B(ΦB) P̃SB(µ\n2\nQ,O)+\n\n∫\ndΦR H(ΦR) PSR(tR,O) (2.1)\n\nwith the familiar B function defined as B = B+V+ IK, and the hard remainder H = R−DK.\nThe matched parton shower P̃SB(µ\n\n2\nQ,O) is defined through P̃SB(µ\n\n2\nQ,O) = ∆DK(µ\n\n2\nQ, tc)O(ΦB) +∫\n\ndt ′ DK\nB ∆DK(µ\n\n2, t ′)PSR(t ′,O) with a continuing standard parton shower PSn(t,O) operating on the\nn-parton configuration with starting scale t. The splitting kernels of the matched shower are the\nDK and the DK are their integrated version. The resummation region is limited by µQ. The various\napproaches now differ in their choices of DK and µQ, they are detailed in Tab. 1. While MC@NLO\n\nretains the parton shower’s splitting function and resummation region definition, POWHEG uses the\npartitioned real emission matrix element as resummation kernel and fills the entire available phase\nspace. Both cases can lead to articfacts when large NLO corrections are present as, upon expansion\nof the matched parton shower emission, the emission spectrum is enhanced by a factor of B/B in\nthe resummation region. In POWHEG, these effects can be mitigated using the hfact-treatment\n[32]. Its results are shown in Fig. 1.\n\nA major recent development for processes with internal resonances is discussed thereafter has\nbeen published in [33, 34, 35, 36]. Therein, the inherent subtractions and momentum maps have\n\nMC@NLO POWHEG\n\nDK B · K̃PS R\nµ2\n\nQ µ2\nF Shad\n\nTable 1: Choices of resummation kernels and the size of the resummation region in POWHEG- and\nMC@NLO-type matching algorithms.\n\n1\n\n\n\nP\no\nS\n(\nC\nO\nR\nF\nU\n2\n0\n1\n7\n)\n1\n1\n0\n\nParton shower matching and merging Marek Schönherr\n\nb\n\nb\n\nb\n\nb\n\nb\n\nb\n\nb\n\nb\n\nb\n\nb\n\nb\n\nb\n\nb\n\nb\n\nb\n\nb\n\nb\n\nb\n\nb\n\nb\n\nb\n\nb\n\nb\n\np⊥(first jet)\n\np⊥(second jet)\n\np⊥(third jet)\n\nSherpa+BlackHat\nW+1,2,3 jets\n\nATLAS datab\n\nNLO\n\nµF/R = µ/2 . . . 2µ\n\nMC@NLO PL\n\nµQ = µ/\n√\n2 . . .\n\n√\n2µ\n\n10−2\n\n10−1\n\n1\n\n10 1\n\nJet transverse momenta\n\nd\nσ\n/\nd\np\n\n⊥\n[p\nb\n/\nG\neV\n\n]\n\nb b b b b b b b b b\n\n0.5\n\n1\n\n1.5\n\nM\nC\n/\nd\na\nta\n\nb b b b b b b\n\n0.5\n\n1\n\n1.5\n\nM\nC\n/\nd\na\nta\n\nb b b b b b\n\n50 100 150 200 250 300\n\n0.5\n\n1\n\n1.5\n\np⊥ [GeV]\n\nM\nC\n/\nd\na\nta\n\nFigure 1: Left: Comparison of the pT spectrum of the Higgs boson (mh = 400 GeV) in gluon fusion with\nMC@NLO and POWHEG, with and without the hfact treatment. Figure taken from [32]. Right: Parton\nshower matched results for W +n jets production using an MC@NLO-like techniques generated by SHERPA.\nFigure taken from [27].\n\n10−2\n\n10−1\n\nd\nσ\n/d\n\nm\nW\n\nj\nB\n[p\nb\n/G\n\neV\n]\n\n8 TeV\n\nd\nσ\n/d\n\nσ\nb\nb̄\n4\nℓ\n\nd\nσ\n/d\n\nm\nW\n\nj\nB\n[p\nb\n/G\n\neV\n]\n\n8 TeV\n\nd\nσ\n/d\n\nσ\nb\nb̄\n4\nℓ\n\nbb̄4ℓ\nres-default\n\nres-off\n\nres-guess\n\nmWjB\n[GeV]\n\n0.5\n\n1.0\n\n1.5\n\n150 160 170 180 190 200\n\n10−4\n\n10−3\n\n10−2\n\nd\nσ\n/d\n\nm\nlj\nB\n[p\nb\n/G\n\neV\n]\n\n8 TeV\n\nd\nσ\n/d\n\nσ\nb\nb̄\n4\nℓ\n\nd\nσ\n/d\n\nm\nlj\nB\n[p\nb\n/G\n\neV\n]\n\n8 TeV\n\nd\nσ\n/d\n\nσ\nb\nb̄\n4\nℓ\n\nbb̄4ℓ\nres-default\n\nres-off\n\nres-guess\n\nmljB\n[GeV]\n\n0.8\n\n1.0\n\n1.2\n\n0 50 100 150 200 250 300 350\n\nFigure 2: Size of the distortion of resonance shape in tt̄ production if not treated properly. Figure taken\nfrom [35].\n\nbeen changed such that the matched results preserves the shape of the internal resonance and the\nmatching to the parton shower does not introduce distortions. Fig. 2 shows that for important\nobservables these distortions can amount to more than 50%, if the matching is unaware of the\ninternal resonance.\n\nFinally, a small class of NLO EW corrections has also been matched to a QED parton shower\n[37, 38, 39]. Here, an interleaving with the NLO QCD corrections and a resonance aware matching\nis essential. Selected results are shown in Fig. 3.\n\n2\n\n\n\nP\no\nS\n(\nC\nO\nR\nF\nU\n2\n0\n1\n7\n)\n1\n1\n0\n\nParton shower matching and merging Marek Schönherr\n\n100\n\n101\n\n102\n\n103\n\nd\nσ\n/d\nm\n\nll\n[p\nb\n/G\n\neV\n]\n\nPOWHEG QCDxEW + Pythia8\n\nLO (w/o Pythia) Sdef SM\n\n60 70 80 90 100 110\n\nmll [GeV]\n\n−20\n\n0\n\n20\n\n40\n\n60\n\n80\n\n100\n\n120\n\nδ[\n%\n]\n\n60 70 80 90 100 110\n\nmll [GeV]\n\n−3\n\n−2\n\n−1\n\n0\n\n1\n\n2\n\n3\n\n4\n\nδ[\n%\n]\n\nPOWHEG QCDxEW + Pythia8\n\nSM Sres Sq BOX\n\nFigure 3: NLO QCD+EW parton shower matched calculation for W production. The corrections crucially\ndepend on the resonance awareness of the matching algorithm. Figure taken from [39].\n\n10−3\n\n10−2\n\n10−1\n\n100\n\nd\nσ\n/d\n\np\nH T\n[p\nb\n/G\n\neV\n]\n\nR\nat\nio\n\npH\n\nT\n[GeV]\n\nd\nσ\n/d\n\np\nH T\n[p\nb\n/G\n\neV\n]\n\nR\nat\nio\n\nNNLOPS\n\nHQT\n\n0.6\n1.0\n1.4\n\n0 50 100 150 200 250 300\n\nSherpa+BlackHatSherpa+BlackHatSherpa+BlackHat\n\nLOPS2UN\nMC@NLO\nNNLO\n\n = 7 TeVs\n<120 GeV\n\nll\n60 GeV<m\n\nll<2m\nR/F\n\nµ/2< ll m\n\nll<2m\nQ\n\nµ/2< ll m\n\n = 7 TeVs\n<120 GeV\n\nll\n60 GeV<m\n\nll<2m\nR/F\n\nµ/2< ll m\n\nll<2m\nQ\n\nµ/2< ll m\n\n = 7 TeVs\n<120 GeV\n\nll\n60 GeV<m\n\nll<2m\nR/F\n\nµ/2< ll m\n\nll<2m\nQ\n\nµ/2< ll m\n\n [p\nb/\n\nG\neV\n\n]\n-\n\nT,\ne\n\n/d\np\n\nσd\n\n1\n\n10\n\n210\n\nR\nat\n\nio\n to\n\n N\nN\n\nLO\n\n0.9\n\n1\n\n1.1\n\n [GeV]-T,e\np\n\n0 10 20 30 40 50 60 70 80 90 100R\nat\n\nio\n to\n\n N\nN\n\nLO\n\n0.9\n\n1\n\n1.1\n\n [GeV]-T,e\np\n\n0 10 20 30 40 50 60 70 80 90 100R\nat\n\nio\n to\n\n N\nN\n\nLO\n\n0.9\n\n1\n\n1.1\n\n [GeV]-T,e\np\n\n0 10 20 30 40 50 60 70 80 90 100R\nat\n\nio\n to\n\n N\nN\n\nLO\n\n0.9\n\n1\n\n1.1\n\n [GeV]-T,e\np\n\n0 10 20 30 40 50 60 70 80 90 100\n\nFigure 4: NNLOPS matched results for the Higgs boson pT in gluon fusion with MiNLO (left) and the pTof\nthe electron in Drell-Yan. Figures taken from [15] and [41].\n\n3. Matching next-to-next-to-leading order matrix elements to parton showers\n\nRecently, also NNLO computations have been matched to parton showers The available im-\nplementations, however, are currently limited to singlet production where the logarithmic accu-\nracy of the parton showers is sufficient for this task. Three unique formulations exist: MiNLO\n\n[40, 15, 16, 17, 18], UN2LOPS [41, 42] and GENEVA [19], employing very different matching algo-\nrithms. Selected results are shown in Fig. 4.\n\n4. Multijet merging at next-to-leading order accuracy\n\nWhile LOPS, NLOPS and NNLOPS describe observables dominated by topologies of a single\njet multiplicity to the given accuracy, a large and important class of observables at LHC receives\nsignificant contributions from multiple jet multiplicities. Examples are HT and pTspectra as well as\nazimuthal separations. Here, the accuracy of the above described calculations rapidly deteriorates.\n\n3\n\n\n\nP\no\nS\n(\nC\nO\nR\nF\nU\n2\n0\n1\n7\n)\n1\n1\n0\n\nParton shower matching and merging Marek Schönherr\n\nSherpa+OpenLoops\n\nMEPS@NLO\n1.65 × MEPS@LO\n\nS-MC@NLO\n\n10−6\n\n10−5\n\n10−4\n\n10−3\n\nTotal transverse energy\n\nd\nσ\n\n/\nd\n\nH\nto\n\nt\nT\n\n[p\nb/\n\nG\neV\n\n]\n\n0.5\n\n1\n\n1.5\n\nR\nat\n\nio\nto\n\nM\nE\n\nPS\n@\n\nN\nL\n\nO\n\n0 200 400 600 800 1000 1200\n0\n\n0.2\n\n0.4\n\n0.6\n\n0.8\ntt̄ + 0 jets excl.\ntt̄ + 1 jet excl.\ntt̄ + 2 jets incl.\n\nHtot\nT [GeV]\n\nR\nat\n\nio\nto\n\nM\nE\n\nPS\n@\n\nN\nL\n\nO\n\nSherpa+OpenLoops\n\nMEPS@NLO\n1.65 × MEPS@LO\n\nS-MC@NLO\n\n10−6\n\n10−5\n\n10−4\n\n10−3\n\n10−2\nTransverse momentum of reconstructed top quark\n\nd\nσ\n\n/\nd\n\np T\n[p\n\nb/\nG\n\neV\n]\n\n0.5\n\n1\n\n1.5\n\nR\nat\n\nio\nto\n\nM\nE\n\nPS\n@\n\nN\nL\n\nO\n\n0 100 200 300 400 500 600\n0\n\n0.2\n\n0.4\n\n0.6\n\n0.8 tt̄ + 0 jets excl. tt̄ + 1 jet excl.\ntt̄ + 2 jets incl.\n\npT (top) [GeV]\n\nR\nat\n\nio\nto\n\nM\nE\n\nPS\n@\n\nN\nL\n\nO\n\nFigure 5: Total transverse energy and top quark transverse momentum deecribed with MEPS@LO and\nMEPS@NLO with reduced theoretical uncertainty. Figures taken from [62].\n\nMultijet merging techniques were introduced to consistently combine calculations from various\nsuccessive jet multiplicities at the highest available precision. At the same time, multijet merged\nevent samples provide the LHC experiments with the largest freedom of projecting these samples\nonto as many observables as possible without the loss of accuracy. Available multijet merging\nmethods, be it at LO or NLO accuracy, fall into two type of algorithms: CKKW-type and MLM-\ntype.\n\nBoth algoithms define a resultion criterion Qcut, which separates n-jet production from (n+1)-\njet production. In this way the procedure can be iterated, adding jet multiplicities as long as it com-\nputationally feasible. While the MLM-type algorithms merge either jet multiplicities described at\nLO (MLM [43]) or NLO (FxFx [44]) only, the CKKW-type algorithms can merge successively ei-\nther LO matrix elements to LO matrix elements (MEPS@LO [45, 46, 47, 48, 49, 50, 51, 52]), NLO\nmatrix elements to LO matrix elements (MENLOPS [53, 54, 55, 56, 36]), or NLO matrix elements\nto NLO matrix elements (MEPS@NLO [57, 55, 52, 58, 51, 59, 60, 61, 62, 64, 63]). Example results\nare shown in Figs. 5 and 6.\n\nFurther, loop-induced process form an important class of processes measured at the LHC.\nTheir theoretical description is complicated that the LO calculation already involves a loop com-\nputation. Nonetheless, additional jet activity is also prevalent in this class and a multijet merged\ncalculation is desirable. Therefore, two different ansatzes have been persued. In cases where an\neffective theory which integrates out the loop exists, the calculation is performed in that effective\ntheory (which has only LO complexity) and then reweighted to include the corrections due to the\nexact loop dynamics [66, 67] . In this way, a NLO merging in the effective theory including Born\nlevel loop corrections are feasible.\n\nOn the other hand, at LO accuracy, direct loop-induced calculations can be merged using a\ntechnique dubbed MEPS@LOOP2 [69, 72]. Fig. 7 shows example results.\n\nFinally, approximate NLO EW corrections were incorporated in NLO multijet merging meth-\n\n4\n\n\n\nP\no\nS\n(\nC\nO\nR\nF\nU\n2\n0\n1\n7\n)\n1\n1\n0\n\nParton shower matching and merging Marek Schönherr\n\n210 310\n\n[fb\n / \n\nG\neV\n\n]\nγγ\n\n/d\nm\n\nσd\n\n2−10\n\n1−10\n\n1\n\n10\n\n210\n\n310\n\n410\nData + stat. unc.\nTotal exp. uncertainty\n\nNNLO (NNLO)γ2\nSHERPA 2.2.1 (ME+PS at NLO)\n\n-1= 8 TeV, 20.2 fbsATLAS\n\n0 100 200\n0\n\n100\n\n200\n\n[GeV]γγm\n210 310Th\n\neo\nry\n\n / \nD\n\nat\na\n\n0.5\n\n1\n\n1.5\n10 210\n\n[fb\n / \n\nG\neV\n\n]\nγγ\n\nT,\n/d\n\np\nσd\n\n2−10\n\n1−10\n\n1\n\n10\n\n210\n\n310\n\n410 Data + stat. unc.\nTotal exp. uncertainty\n\nNNLO (NNLO)γ2\nSHERPA 2.2.1 (ME+PS at NLO)\n\n-1= 8 TeV, 20.2 fbsATLAS\n\n0 50\n0\n\n200\n\n400\n\n[GeV]\nγγT,\n\np10 210\n\nTh\neo\n\nry\n / \n\nD\nat\n\na\n\n0.5\n\n1\n\n1.5\n\nFigure 6: Diphoton invariant mass and pair transverse momentum in photon pair production with\nMEPS@NLO compared to ATLAS data. Figures taken from [65].\n\nSh\ner\n\npa\n+G\n\no\nSa\n\nm\n\nHEFT central\nSM central\nHEFT up\nSM up\nHEFT down\nSM down\n\n10−1\n\n1\n\n10 1\n\n10 2\n\nd\nσ\n\n/d\np T\n\n[p\nb/\n\nG\neV\n\n]\n\n0 100 200 300 400 500\n\n0.5\n\n1\n\n1.5\n\npT(γ1γ2) [GeV]\n\nR\nat\n\nio\n\n10−3\n\n10−2\n\n10−1\n\nd\nσ\n\n/d\n∆\n\nφ\n(l\n\nl,\nE\n\nm\nis\n\ns\nT\n\n)\n[p\n\nb]\n\nSherpa+OpenLoops\n\nMEPS@NLO [scale variations]\n0-jet exclusive\n\nMEPS@Loop2 [scale variations]\n\nMEPS@Loop2 [k-factor variations]\n0-jet exclusive\n\n2.6 2.7 2.8 2.9 3.0 3.1\n∆φ(ll, Emiss\n\nT )\n\n0.0\n\n0.2\n\n0.4\n\n0.6\n\n0.8\n\nR\nat\n\nio\nto\n\nin\nc.\n\nsa\nm\n\npl\ne\n\nFigure 7: Left: Top mass corrections in an NLO multijet merged calculation of the diphoton pT spectrum\nin Higgs production in gluon fusion. Right: NLO qq̄- and LO loop-induced gg-induced contribution to Zh\nassociated production. Figure taken from [72].\n\nods in [33].\n\n5. Conclusions\n\nAll processes of relevance to LHC analyses are available at least at NLOPS accuracy. Key\nprocesses like W , Z and h production are even known to NNLOPS accuracy. To also merge non-\ncolour-singlet process at this accuracy to parton showers, the logarithmic accuracy of the latter\nneed to be improved first [73, 74, 75, 76].\n\n5\n\n\n\nP\no\nS\n(\nC\nO\nR\nF\nU\n2\n0\n1\n7\n)\n1\n1\n0\n\nParton shower matching and merging Marek Schönherr\n\nOn another, almost orthogonal direction, the recent progress in the automation of NLO EW\ncorrections [77, 78, 33, 79, 80, 81, 82, 83, 36] should be universally matched to parton showers and\nincluded in the standard event simulation. Current, approximate methods [33] are only targeted\nat large-pT physics. At the same time, developments in including EW effects into parton showers\n[84, 85, 86, 87, 88] are not only relevant for future colliders at energies up to 100 TeV, but also\noffer a way of extending multijet merging to include jet emissions through hadronically decaying\nvector boson production as well.\n\nReferences\n\n[1] T. Sjöstrand et al., Comput. Phys. Commun. 191 (2015) 159 doi:10.1016/j.cpc.2015.01.024\n[arXiv:1410.3012 [hep-ph]].\n\n[2] M. Bahr et al., Eur. Phys. J. C 58 (2008) 639 doi:10.1140/epjc/s10052-008-0798-9 [arXiv:0803.0883\n[hep-ph]].\n\n[3] J. Bellm et al., arXiv:1705.06919 [hep-ph].\n\n[4] T. Gleisberg, S. Hoeche, F. Krauss, M. Schonherr, S. Schumann, F. Siegert and J. Winter, JHEP 0902\n(2009) 007 doi:10.1088/1126-6708/2009/02/007 [arXiv:0811.4622 [hep-ph]].\n\n[5] F. Krauss, R. Kuhn and G. Soff, JHEP 0202 (2002) 044 doi:10.1088/1126-6708/2002/02/044\n[hep-ph/0109036].\n\n[6] T. Gleisberg and S. 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Comparison of the \\pT\\ spectrum of the Higgs boson ($m_h=400\\,\\GeV$) in gluon fusion with \\MCatNLO and \\Powheg, with and without the \\texttt{hfact} treatment. Figure taken from \\cite{arXiv:0812.0578}. \\textbf{Right:} Parton shower matched results for $W+n$\\,jets production using an \\MCatNLO-like techniques generated by \\Sherpa. Figure taken from \\cite{arXiv:1201.5882}.","source":"arxiv","key":"26473cc61d9cccf7651f610304279a11","url":"https://inspirehep.net/files/26473cc61d9cccf7651f610304279a11"},{"filename":"wnj_fig_1a.png","caption":"\\textbf{Left:} Comparison of the \\pT\\ spectrum of the Higgs boson ($m_h=400\\,\\GeV$) in gluon fusion with \\MCatNLO and \\Powheg, with and without the \\texttt{hfact} treatment. Figure taken from \\cite{arXiv:0812.0578}. \\textbf{Right:} Parton shower matched results for $W+n$\\,jets production using an \\MCatNLO-like techniques generated by \\Sherpa. Figure taken from \\cite{arXiv:1201.5882}.","source":"arxiv","key":"e991a5f146fff7e776c17a2b209c8535","url":"https://inspirehep.net/files/e991a5f146fff7e776c17a2b209c8535"},{"filename":"wnj_fig_1b.png","caption":"\\textbf{Left:} Comparison of the \\pT\\ spectrum of the Higgs boson ($m_h=400\\,\\GeV$) in gluon fusion with \\MCatNLO and \\Powheg, with and without the \\texttt{hfact} treatment. Figure taken from \\cite{arXiv:0812.0578}. \\textbf{Right:} Parton shower matched results for $W+n$\\,jets production using an \\MCatNLO-like techniques generated by \\Sherpa. Figure taken from \\cite{arXiv:1201.5882}.","source":"arxiv","key":"6f5cf7579488182b5ebb1503da2c3ba0","url":"https://inspirehep.net/files/6f5cf7579488182b5ebb1503da2c3ba0"},{"filename":"wnj_fig_1c.png","caption":"\\textbf{Left:} Comparison of the \\pT\\ spectrum of the Higgs boson ($m_h=400\\,\\GeV$) in gluon fusion with \\MCatNLO and \\Powheg, with and without the \\texttt{hfact} treatment. Figure taken from \\cite{arXiv:0812.0578}. \\textbf{Right:} Parton shower matched results for $W+n$\\,jets production using an \\MCatNLO-like techniques generated by \\Sherpa. Figure taken from \\cite{arXiv:1201.5882}.","source":"arxiv","key":"91c7d2e7e0a7ef1a833a6f5818f7134c","url":"https://inspirehep.net/files/91c7d2e7e0a7ef1a833a6f5818f7134c"},{"filename":"wnj_fig_1d.png","caption":"\\textbf{Left:} Comparison of the \\pT\\ spectrum of the Higgs boson ($m_h=400\\,\\GeV$) in gluon fusion with \\MCatNLO and \\Powheg, with and without the \\texttt{hfact} treatment. Figure taken from \\cite{arXiv:0812.0578}. \\textbf{Right:} Parton shower matched results for $W+n$\\,jets production using an \\MCatNLO-like techniques generated by \\Sherpa. Figure taken from \\cite{arXiv:1201.5882}.","source":"arxiv","key":"3551d07119c70f5c06707adbab6df204","url":"https://inspirehep.net/files/3551d07119c70f5c06707adbab6df204"},{"filename":"8TeV_res-allrad_nores_PY8_m_w_jbot-cut1-pyMEC1.png","caption":"Size of the distortion of resonance shape in $t\\bar{t}$ production if not treated properly. Figure taken from \\cite{arXiv:1607.04538}.","source":"arxiv","key":"a496cd848844b8a65e5adb9ac771a66b","url":"https://inspirehep.net/files/a496cd848844b8a65e5adb9ac771a66b"},{"filename":"top_pt.png","caption":"Total transverse energy and top quark transverse momentum deecribed with \\protect\\MEPS and \\protect\\MEPSatNLO with reduced theoretical uncertainty. Figures taken from \\cite{arXiv:1402.6293}.","source":"arxiv","key":"f0ac93c7b540a27e0ce560134a75fc7a","url":"https://inspirehep.net/files/f0ac93c7b540a27e0ce560134a75fc7a"},{"filename":"qcdew_born_veto.png","caption":"NLO QCD+EW parton shower matched calculation for $W$ production. The corrections crucially depend on the resonance awareness of the matching algorithm. Figure taken from \\cite{arXiv:1612.04292}.","source":"arxiv","key":"3de60fdde6a34d3e83923873397bbd3d","url":"https://inspirehep.net/files/3de60fdde6a34d3e83923873397bbd3d"},{"filename":"fig_1b.png","caption":"\\textbf{Left:} Comparison of the \\pT\\ spectrum of the Higgs boson ($m_h=400\\,\\GeV$) in gluon fusion with \\MCatNLO and \\Powheg, with and without the \\texttt{hfact} treatment. Figure taken from \\cite{arXiv:0812.0578}. \\textbf{Right:} Parton shower matched results for $W+n$\\,jets production using an \\MCatNLO-like techniques generated by \\Sherpa. Figure taken from \\cite{arXiv:1201.5882}.","source":"arxiv","key":"cd97a659015577caf29937af35887be7","url":"https://inspirehep.net/files/cd97a659015577caf29937af35887be7"},{"filename":"fig_1c.png","caption":"\\textbf{Left:} Comparison of the \\pT\\ spectrum of the Higgs boson ($m_h=400\\,\\GeV$) in gluon fusion with \\MCatNLO and \\Powheg, with and without the \\texttt{hfact} treatment. Figure taken from \\cite{arXiv:0812.0578}. \\textbf{Right:} Parton shower matched results for $W+n$\\,jets production using an \\MCatNLO-like techniques generated by \\Sherpa. Figure taken from \\cite{arXiv:1201.5882}.","source":"arxiv","key":"eb14ad7ff93919fd7eeef970283e30df","url":"https://inspirehep.net/files/eb14ad7ff93919fd7eeef970283e30df"},{"filename":"pTl.png","caption":"\\protect\\NNLOPS matched results for the Higgs boson \\pT\\ in gluon fusion with \\MINLO (left) and the \\pT of the electron in Drell-Yan. Figures taken from \\cite{arXiv:1309.0017} and \\cite{arXiv:1405.3607}.","source":"arxiv","key":"f3f1b39d99076a29ca351bfaf88966b7","url":"https://inspirehep.net/files/f3f1b39d99076a29ca351bfaf88966b7"},{"filename":"fig_1a.png","caption":"\\textbf{Left:} Comparison of the \\pT\\ spectrum of the Higgs boson ($m_h=400\\,\\GeV$) in gluon fusion with \\MCatNLO and \\Powheg, with and without the \\texttt{hfact} treatment. Figure taken from \\cite{arXiv:0812.0578}. \\textbf{Right:} Parton shower matched results for $W+n$\\,jets production using an \\MCatNLO-like techniques generated by \\Sherpa. Figure taken from \\cite{arXiv:1201.5882}.","source":"arxiv","key":"b9c274ba100706b9ea8e51a3a87405c0","url":"https://inspirehep.net/files/b9c274ba100706b9ea8e51a3a87405c0"},{"filename":"ttbar_ht_ratio1.png","caption":"Total transverse energy and top quark transverse momentum deecribed with \\protect\\MEPS and \\protect\\MEPSatNLO with reduced theoretical uncertainty. Figures taken from \\cite{arXiv:1402.6293}.","source":"arxiv","key":"b80cc75fc95fa67b7236273d5732375a","url":"https://inspirehep.net/files/b80cc75fc95fa67b7236273d5732375a"},{"filename":"top_pt_ratio2.png","caption":"Total transverse energy and top quark transverse momentum deecribed with \\protect\\MEPS and \\protect\\MEPSatNLO with reduced theoretical uncertainty. Figures taken from \\cite{arXiv:1402.6293}.","source":"arxiv","key":"d16124415de71be3b77a90e880eb62ee","url":"https://inspirehep.net/files/d16124415de71be3b77a90e880eb62ee"},{"filename":"fig_1d.png","caption":"\\textbf{Left:} Comparison of the \\pT\\ spectrum of the Higgs boson ($m_h=400\\,\\GeV$) in gluon fusion with \\MCatNLO and \\Powheg, with and without the \\texttt{hfact} treatment. Figure taken from \\cite{arXiv:0812.0578}. \\textbf{Right:} Parton shower matched results for $W+n$\\,jets production using an \\MCatNLO-like techniques generated by \\Sherpa. Figure taken from \\cite{arXiv:1201.5882}.","source":"arxiv","key":"433176227624196625aae10633b27f5d","url":"https://inspirehep.net/files/433176227624196625aae10633b27f5d"},{"filename":"ht_ratio2.png","caption":"Total transverse energy and top quark transverse momentum deecribed with \\protect\\MEPS and \\protect\\MEPSatNLO with reduced theoretical uncertainty. Figures taken from \\cite{arXiv:1402.6293}.","source":"arxiv","key":"df6ffe8b7a9eedad0864446b2ef8e791","url":"https://inspirehep.net/files/df6ffe8b7a9eedad0864446b2ef8e791"},{"filename":"ttbar_top_pt_ratio2.png","caption":"Total transverse energy and top quark transverse momentum deecribed with \\protect\\MEPS and \\protect\\MEPSatNLO with reduced theoretical uncertainty. Figures taken from \\cite{arXiv:1402.6293}.","source":"arxiv","key":"19209d752e611b9b7366c2113d0f30fb","url":"https://inspirehep.net/files/19209d752e611b9b7366c2113d0f30fb"},{"filename":"ht.png","caption":"Total transverse energy and top quark transverse momentum deecribed with \\protect\\MEPS and \\protect\\MEPSatNLO with reduced theoretical uncertainty. Figures taken from \\cite{arXiv:1402.6293}.","source":"arxiv","key":"de7748c1104127e270e67411d2a1f813","url":"https://inspirehep.net/files/de7748c1104127e270e67411d2a1f813"},{"filename":"top_pt_ratio1.png","caption":"Total transverse energy and top quark transverse momentum deecribed with \\protect\\MEPS and \\protect\\MEPSatNLO with reduced theoretical uncertainty. Figures taken from \\cite{arXiv:1402.6293}.","source":"arxiv","key":"8a92b0397af8465c4be29288ae38bcdc","url":"https://inspirehep.net/files/8a92b0397af8465c4be29288ae38bcdc"},{"filename":"ht_ratio1.png","caption":"Total transverse energy and top quark transverse momentum deecribed with \\protect\\MEPS and \\protect\\MEPSatNLO with reduced theoretical uncertainty. Figures taken from \\cite{arXiv:1402.6293}.","source":"arxiv","key":"ed3af3b011e7f3ca535c77a3c28c8de8","url":"https://inspirehep.net/files/ed3af3b011e7f3ca535c77a3c28c8de8"},{"filename":"hz_dphi_metc.png","caption":"\\textbf{Left:} Top mass corrections in an NLO multijet merged calculation of the diphoton \\pT\\ spectrum in Higgs production in gluon fusion. \\textbf{Right:} NLO $q\\bar{q}$- and LO loop-induced $gg$-induced contribution to $Zh$ associated production. Figure taken from \\cite{arXiv:1509.01597}.","source":"arxiv","key":"c0ab182060374267b4713d2aa1b70d3c","url":"https://inspirehep.net/files/c0ab182060374267b4713d2aa1b70d3c"}],"legacy_version":"20180924140722.0","inspire_categories":[{"term":"Phenomenology-HEP","source":"arxiv"},{"term":"Phenomenology-HEP"}],"urls":[{"description":"PoS server","value":"https://pos.sissa.it/318/110/pdf"}],"first_author":{"affiliations_identifiers":[{"schema":"ROR","value":"https://ror.org/01ggx4157"}],"full_name":"Schönherr, Marek","last_name":"Schönherr","first_name":"Marek","recid":1061205},"control_number":1670813,"dois":[{"source":"bibmatch","value":"10.22323/1.318.0110"}],"document_type":["conference paper"],"texkeys":["Schonherr:2018rlx"],"abstracts":[{"source":"arXiv","value":"With Run-II of the LHC starting its final year of data-taking, high precision theoretical predictions through Monte-Carlo event generators whose uncertainties match that of the recorded data are of highest importance. This talk summarises the progress of the field and highlight a number of recent developments.","abstract_source_suggest":{"input":"arXiv"}}],"primary_arxiv_category":["hep-ph"],"titles":[{"source":"arXiv","title":"Parton shower matching and merging"}],"imprints":[{"date":"2018-04-27","publisher":"SISSA"}],"curated":true},"links":{"bibtex":"https://inspirehep.net/api/literature/1670813?format=bibtex","latex-eu":"https://inspirehep.net/api/literature/1670813?format=latex-eu","latex-us":"https://inspirehep.net/api/literature/1670813?format=latex-us","json":"https://inspirehep.net/api/literature/1670813?format=json","json-expanded":"https://inspirehep.net/api/literature/1670813?format=json-expanded","cv":"https://inspirehep.net/api/literature/1670813?format=cv","citations":"https://inspirehep.net/api/literature/?q=refersto%3Arecid%3A1670813"},"updated":"2023-03-07T00:02:19.128392+00:00","created":"2018-05-01T00:00:00+00:00","id":"1670813"}],"total":25218},"links":{"self":"https://inspirehep.net/api/literature/?q=refersto%3Aarxiv%3A2504.18487&size=10&page=1","next":"https://inspirehep.net/api/literature/?q=refersto%3Aarxiv%3A2504.18487&size=10&page=2","bibtex":"https://inspirehep.net/api/literature/?q=refersto%3Aarxiv%3A2504.18487&size=10&page=1&format=bibtex","latex-eu":"https://inspirehep.net/api/literature/?q=refersto%3Aarxiv%3A2504.18487&size=10&page=1&format=latex-eu","latex-us":"https://inspirehep.net/api/literature/?q=refersto%3Aarxiv%3A2504.18487&size=10&page=1&format=latex-us","json":"https://inspirehep.net/api/literature/?q=refersto%3Aarxiv%3A2504.18487&size=10&page=1&format=json","json-expanded":"https://inspirehep.net/api/literature/?q=refersto%3Aarxiv%3A2504.18487&size=10&page=1&format=json-expanded","cv":"https://inspirehep.net/api/literature/?q=refersto%3Aarxiv%3A2504.18487&size=10&page=1&format=cv"}}