Miriam Kümmel

Ruhr-Universität Bochum

H-index: 48

Europe-Germany

About Miriam Kümmel

Miriam Kümmel, With an exceptional h-index of 48 and a recent h-index of 41 (since 2020), a distinguished researcher at Ruhr-Universität Bochum, specializes in the field of hadron physics.

His recent articles reflect a diverse array of research interests and contributions to the field:

Euclid: Validation of the MontePython forecasting tools

Euclid preparation-XXXIII. Characterization of convolutional neural networks for the identification of galaxy-galaxy strong-lensing events

Euclid preparation-XXXVII. Galaxy colour selections with Euclid and ground photometry for cluster weak-lensing analyses

Euclid preparation

Euclid preparation-XXXV. Covariance model validation for the two-point correlation function of galaxy clusters

Observation of decays to and

Euclid preparation. Measuring detailed galaxy morphologies for Euclid with Machine Learning

Euclid preparation: TBD. The pre-launch Science Ground Segment simulation framework

Miriam Kümmel Information

University	Ruhr-Universität Bochum
Position	___
Citations(all)	9503
Citations(since 2020)	7305
Cited By	1729
hIndex(all)	48
hIndex(since 2020)	41
i10Index(all)	203
i10Index(since 2020)	187
Email	Access Email
University Profile Page	Ruhr-Universität Bochum

Miriam Kümmel Skills & Research Interests

hadron physics

Top articles of Miriam Kümmel

Euclid: Validation of the MontePython forecasting tools

Authors

Santiago Casas,J Lesgourgues,N Schöneberg,VM Sabarish,L Rathmann,M Doerenkamp,M Archidiacono,E Bellini,S Clesse,N Frusciante,M Martinelli,F Pace,D Sapone,Z Sakr,A Blanchard,T Brinckmann,S Camera,C Carbone,S Ilić,K Markovic,V Pettorino,I Tutusaus,N Aghanim,A Amara,L Amendola,N Auricchio,M Baldi,D Bonino,E Branchini,M Brescia,J Brinchmann,V Capobianco,VF Cardone,J Carretero,M Castellano,S Cavuoti,A Cimatti,R Cledassou,G Congedo,L Conversi,Y Copin,L Corcione,F Courbin,M Cropper,H Degaudenzi,J Dinis,M Douspis,F Dubath,X Dupac,S Dusini,S Farrens,M Frailis,E Franceschi,M Fumana,S Galeotta,B Garilli,B Gillis,C Giocoli,A Grazian,F Grupp,L Guzzo,SVH Haugan,F Hormuth,A Hornstrup,K Jahnke,M Kümmel,A Kiessling,M Kilbinger,T Kitching,M Kunz,H Kurki-Suonio,S Ligori,PB Lilje,I Lloro,O Mansutti,O Marggraf,F Marulli,R Massey,E Medinaceli,S Mei,M Meneghetti,E Merlin,G Meylan,M Moresco,L Moscardini,E Munari,S-M Niemi,C Padilla,S Paltani,F Pasian,K Pedersen,WJ Percival,S Pires,G Polenta,M Poncet,LA Popa,F Raison,A Renzi,J Rhodes,G Riccio,E Romelli,M Roncarelli,E Rossetti,R Saglia,B Sartoris,P Schneider,A Secroun,G Seidel,S Serrano,C Sirignano,G Sirri,L Stanco,J-L Starck,C Surace,P Tallada-Crespí,AN Taylor,I Tereno,R Toledo-Moreo,F Torradeflot,EA Valentijn,L Valenziano,T Vassallo,Y Wang,J Weller,G Zamorani,J Zoubian,V Scottez,A Veropalumbo

Journal

Astronomy & Astrophysics

Published Date

2024/2/1

Context. The Euclid mission of the European Space Agency will perform a survey of weak lensing cosmic shear and galaxy clustering in order to constrain cosmological models and fundamental physics.Aims. We expand and adjust the mock Euclid likelihoods of the MontePython software in order to match the exact recipes used in previous Euclid Fisher matrix forecasts for several probes: weak lensing cosmic shear, photometric galaxy clustering, the cross-correlation between the latter observables, and spectroscopic galaxy clustering. We also establish which precision settings are required when running the Einstein–Boltzmann solvers CLASS and CAMB in the context of Euclid.Methods. For the minimal cosmological model, extended to include dynamical dark energy, we perform Fisher matrix forecasts based directly on a numerical evaluation of second derivatives of the likelihood with respect to model …

Euclid preparation-XXXIII. Characterization of convolutional neural networks for the identification of galaxy-galaxy strong-lensing events

Authors

L Leuzzi,M Meneghetti,G Angora,RB Metcalf,L Moscardini,P Rosati,P Bergamini,F Calura,B Clément,R Gavazzi,F Gentile,M Lochner,C Grillo,G Vernardos,N Aghanim,A Amara,L Amendola,N Auricchio,C Bodendorf,D Bonino,E Branchini,M Brescia,J Brinchmann,S Camera,V Capobianco,C Carbone,J Carretero,M Castellano,S Cavuoti,A Cimatti,R Cledassou,G Congedo,CJ Conselice,L Conversi,Y Copin,L Corcione,F Courbin,M Cropper,A Da Silva,H Degaudenzi,J Dinis,F Dubath,X Dupac,S Dusini,S Farrens,S Ferriol,M Frailis,E Franceschi,M Fumana,S Galeotta,B Gillis,C Giocoli,A Grazian,F Grupp,L Guzzo,SVH Haugan,W Holmes,F Hormuth,A Hornstrup,P Hudelot,K Jahnke,M Kümmel,S Kermiche,A Kiessling,T Kitching,M Kunz,H Kurki-Suonio,PB Lilje,I Lloro,E Maiorano,O Mansutti,O Marggraf,K Markovic,F Marulli,R Massey,E Medinaceli,S Mei,M Melchior,Y Mellier,E Merlin,G Meylan,M Moresco,E Munari,S-M Niemi,JW Nightingale,T Nutma,C Padilla,S Paltani,F Pasian,K Pedersen,V Pettorino,S Pires,G Polenta,M Poncet,F Raison,A Renzi,J Rhodes,G Riccio,E Romelli,M Roncarelli,E Rossetti,R Saglia,D Sapone,B Sartoris,P Schneider,A Secroun,G Seidel,S Serrano,C Sirignano,G Sirri,L Stanco,P Tallada-Crespí,AN Taylor,I Tereno,R Toledo-Moreo,F Torradeflot,I Tutusaus,L Valenziano,T Vassallo,Y Wang,J Weller,G Zamorani,J Zoubian,S Andreon,S Bardelli,A Boucaud,E Bozzo,C Colodro-Conde,D Di Ferdinando,M Farina,R Farinelli,J Graciá-Carpio,E Keihänen,V Lindholm,D Maino,N Mauri,C Neissner,M Schirmer,V Scottez,M Tenti,A Tramacere,A Veropalumbo,E Zucca,Y Akrami,V Allevato,C Baccigalupi,M Ballardini,F Bernardeau,A Biviano,S Borgani

Journal

Astronomy & Astrophysics

Published Date

2024/1/1

Forthcoming imaging surveys will increase the number of known galaxy-scale strong lenses by several orders of magnitude. For this to happen, images of billions of galaxies will have to be inspected to identify potential candidates. In this context, deep-learning techniques are particularly suitable for finding patterns in large data sets, and convolutional neural networks (CNNs) in particular can efficiently process large volumes of images. We assess and compare the performance of three network architectures in the classification of strong-lensing systems on the basis of their morphological characteristics. In particular, we implemented a classical CNN architecture, an inception network, and a residual network. We trained and tested our networks on different subsamples of a data set of 40 000 mock images whose characteristics were similar to those expected in the wide survey planned with the ESA mission Euclid …

Euclid preparation-XXXVII. Galaxy colour selections with Euclid and ground photometry for cluster weak-lensing analyses

Authors

GF Lesci,M Sereno,M Radovich,G Castignani,L Bisigello,F Marulli,L Moscardini,L Baumont,G Covone,S Farrens,C Giocoli,L Ingoglia,S Miranda La Hera,M Vannier,A Biviano,S Maurogordato,N Aghanim,A Amara,S Andreon,N Auricchio,M Baldi,S Bardelli,R Bender,C Bodendorf,D Bonino,E Branchini,M Brescia,J Brinchmann,S Camera,V Capobianco,C Carbone,J Carretero,S Casas,FJ Castander,M Castellano,S Cavuoti,A Cimatti,G Congedo,CJ Conselice,L Conversi,Y Copin,L Corcione,F Courbin,HM Courtois,A Da Silva,H Degaudenzi,AM Di Giorgio,J Dinis,F Dubath,CAJ Duncan,X Dupac,S Dusini,M Farina,S Ferriol,P Fosalba,S Fotopoulou,M Frailis,E Franceschi,P Franzetti,M Fumana,S Galeotta,B Garilli,B Gillis,A Grazian,F Grupp,SVH Haugan,I Hook,F Hormuth,A Hornstrup,P Hudelot,K Jahnke,M Kümmel,S Kermiche,A Kiessling,M Kilbinger,B Kubik,M Kunz,H Kurki-Suonio,S Ligori,PB Lilje,V Lindholm,I Lloro,E Maiorano,O Mansutti,O Marggraf,K Markovic,N Martinet,R Massey,E Medinaceli,M Melchior,Y Mellier,M Meneghetti,E Merlin,G Meylan,M Moresco,E Munari,R Nakajima,S-M Niemi,C Padilla,S Paltani,F Pasian,K Pedersen,V Pettorino,S Pires,G Polenta,M Poncet,LA Popa,L Pozzetti,F Raison,R Rebolo,A Renzi,J Rhodes,G Riccio,E Romelli,M Roncarelli,E Rossetti,R Saglia,D Sapone,B Sartoris,M Schirmer,P Schneider,A Secroun,G Seidel,S Serrano,C Sirignano,G Sirri,J Skottfelt,L Stanco,J-L Starck,P Tallada-Crespí,AN Taylor,HI Teplitz,I Tereno,R Toledo-Moreo,F Torradeflot,I Tutusaus,EA Valentijn,L Valenziano,T Vassallo,A Veropalumbo,Y Wang,J Weller,A Zacchei,G Zamorani,J Zoubian,E Zucca,M Bolzonella,E Bozzo,C Colodro-Conde,D Di Ferdinando

Journal

Astronomy & Astrophysics

Published Date

2024/4/1

Aims We derived galaxy colour selections from Euclid and ground-based photometry, aiming to accurately define background galaxy samples in cluster weak-lensing analyses. These selections have been implemented in the Euclid data analysis pipelines for galaxy clusters.Methods Given any set of photometric bands, we developed a method for the calibration of optimal galaxy colour selections that maximises the selection completeness, given a threshold on purity. Such colour selections are expressed as a function of the lens redshift.Results We calibrated galaxy selections using simulated ground-based griz and EuclidYEJEHE photometry. Both selections produce a purity higher than 97%. The griz selection completeness ranges from 30% to 84% in the lens redshift range zl ∈ [0.2, 0.8]. With the full grizYEJEHE selection, the completeness improves by up to 25 percentage points, and the zl range extends …

Euclid preparation

Authors

S Paltani,J Coupon,WG Hartley,A Alvarez-Ayllon,F Dubath,JJ Mohr,M Schirmer,J-C Cuillandre,G Desprez,O Ilbert,K Kuijken,N Aghanim,B Altieri,A Amara,N Auricchio,M Baldi,R Bender,C Bodendorf,D Bonino,E Branchini,M Brescia,J Brinchmann,S Camera,V Capobianco,C Carbone,VF Cardone,J Carretero,FJ Castander,M Castellano,S Cavuoti,R Cledassou,G Congedo,CJ Conselice,L Conversi,Y Copin,L Corcione,F Courbin,M Cropper,A Da Silva,H Degaudenzi,J Dinis,M Douspis,X Dupac,S Dusini,S Farrens,S Ferriol,P Fosalba,M Frailis,E Franceschi,P Franzetti,S Galeotta,B Garilli,W Gillard,B Gillis,C Giocoli,A Grazian,SV Haugan,H Hoekstra,A Hornstrup,P Hudelot,K Jahnke,M Kuemmel,S Kermiche,A Kiessling,M Kilbinger,T Kitching,R Kohley,B Kubik,M Kunz,H Kurki-Suonio,S Ligori,PB Lilje,I Lloro,E Maiorano,O Mansutti,O Marggraf,K Markovic,F Marulli,R Massey,DC Masters,S Maurogordato,HJ McCracken,E Medinaceli,S Mei,M Melchior,M Meneghetti,E Merlin,G Meylan,M Moresco,L Moscardini,E Munari,S-M Niemi,J Nightingale,C Padilla,F Pasian,K Pedersen,WJ Percival,V Pettorino,G Polenta,M Poncet,LA Popa,F Raison,R Rebolo,A Renzi,J Rhodes,G Riccio,E Romelli,M Roncarelli,E Rossetti,R Saglia,D Sapone,B Sartoris,P Schneider,A Secroun,C Sirignano,G Sirri,J Skottfelt,L Stanco,J-L Starck,C Surace,P Tallada-Crespi,I Tereno,R Toledo-Moreo,F Torradeflot,I Tutusaus,EA Valentijn,L Valenziano,T Vassallo,Y Wang,G Zamorani,J Zoubian,S Andreon,H Aussel,S Bardelli,M Bolzonella,A Boucaud,D Di Ferdinando,M Farina,J Gracia-Carpio,V Lindholm,D Maino,N Mauri,C Neissner,V Scottez,E Zucca,C Baccigalupi,M Ballardini,A Biviano,A Blanchard,S Borgani

Journal

Astronomy & Astrophysics

Published Date

2024/1/16

The technique of photometric redshifts has become essential for the exploitation of multi-band extragalactic surveys. While the requirements on photometric redshifts for the study of galaxy evolution mostly pertain to the precision and to the fraction of outliers, the most stringent requirement in their use in cosmology is on the accuracy, with a level of bias at the sub-percent level for the Euclid cosmology mission. A separate, and challenging, calibration process is needed to control the bias at this level of accuracy. The bias in photometric redshifts has several distinct origins that may not always be easily overcome. We identify here one source of bias linked to the spatial or time variability of the passbands used to determine the photometric colours of galaxies. We first quantified the effect as observed on several well-known photometric cameras, and found in particular that, due to the properties of optical filters, the redshifts of off-axis sources are usually overestimated. We show using simple simulations that the detailed and complex changes in the shape can be mostly ignored and that it is sufficient to know the mean wavelength of the passbands of each photometric observation to correct almost exactly for this bias; the key point is that this mean wavelength is independent of the spectral energy distribution of the source. We use this property to propose a correction that can be computationally efficiently implemented in some photometric-redshift algorithms, in particular template-fitting. We verified that our algorithm, implemented in the new photometric-redshift code Phosphoros, can effectively reduce the bias in photometric redshifts on real data using …

Euclid preparation-XXXV. Covariance model validation for the two-point correlation function of galaxy clusters

Authors

Euclid Collaboration,A Fumagalli,A Saro,S Borgani,T Castro,M Costanzi

Published Date

2024/1/10

Aims We validate a semi-analytical model for the covariance of the real-space two-point correlation function of galaxy clusters. Methods Using 1000 PINOCCHIO light cones mimicking the expected Euclid sample of galaxy clusters, we calibrated a simple model to accurately describe the clustering covariance. Then, we used this model to quantify the likelihood-analysis response to variations in the covariance, and we investigated the impact of a cosmology-dependent matrix at the level of statistics expected for the Euclid survey of galaxy clusters. Results We find that a Gaussian model with Poissonian shot-noise does not correctly predict the covariance of the two-point correlation function of galaxy clusters. By introducing a few additional parameters fitted from simulations, the proposed model reproduces the numerical covariance with an accuracy of 10%, with differences of about 5% on the figure of merit of the …

Observation of decays to and

Authors

M Ablikim,MN Achasov,P Adlarson,S Ahmed,M Albrecht,R Aliberti,A Amoroso,MR An,Q An,XH Bai,Y Bai,O Bakina,R Baldini Ferroli,I Balossino,Y Ban,K Begzsuren,N Berger,M Bertani,D Bettoni,F Bianchi,J Bloms,A Bortone,I Boyko,RA Briere,H Cai,X Cai,A Calcaterra,GF Cao,N Cao,SA Cetin,JF Chang,WL Chang,DY Chen,G Chen,HS Chen,ML Chen,SJ Chen,XR Chen,YB Chen,ZJ Chen,WS Cheng,G Cibinetto,F Cossio,XF Cui,HL Dai,JP Dai,XC Dai,A Dbeyssi,RE de Boer,D Dedovich,ZY Deng,A Denig,I Denysenko,M Destefanis,F De Mori,Y Ding,C Dong,J Dong,LY Dong,MY Dong,X Dong,SX Du,YL Fan,J Fang,SS Fang,Y Fang,R Farinelli,L Fava,F Feldbauer,G Felici,CQ Feng,JH Feng,M Fritsch,CD Fu,Y Gao,YG Gao,I Garzia,PT Ge,C Geng,EM Gersabeck,K Goetzen,L Gong,WX Gong,W Gradl,M Greco,LM Gu,MH Gu,S Gu,YT Gu,CY Guan,AQ Guo,LB Guo,RP Guo,YP Guo,A Guskov,TT Han,WY Han,XQ Hao,FA Harris,H Hüsken,KL He,FH Heinsius,CH Heinz,T Held,YK Heng,C Herold,M Himmelreich,T Holtmann,YR Hou,ZL Hou,HM Hu,JF Hu,T Hu,Y Hu,GS Huang,LQ Huang,XT Huang,YP Huang,Z Huang,T Hussain,W Ikegami Andersson,W Imoehl,M Irshad,S Jaeger,S Janchiv,Q Ji,QP Ji,XB Ji,XL Ji,HB Jiang,XS Jiang,JB Jiao,Z Jiao,S Jin,Y Jin,T Johansson,N Kalantar-Nayestanaki,XS Kang,R Kappert,M Kavatsyuk,BC Ke,IK Keshk,A Khoukaz,P Kiese,R Kiuchi,R Kliemt,L Koch,OB Kolcu,B Kopf,M Kuemmel

Journal

Physical Review D

Published Date

2024/3/18

Using a data sample of 4.481× 10 8 ψ (3686) events collected with the BESIII detector, we report the first observation of the four-lepton-decays J/ψ→ e+ e− e+ e− and J/ψ→ e+ e− μ+ μ− utilizing the process ψ (3686)→ π+ π− J/ψ. The branching fractions are determined to be [5.48±0.31 (stat)±0.45 (syst)]× 10− 5 and [3.53±0.22 (stat)±0.13 (syst)]× 10− 5, respectively. The results are consistent with theoretical predictions. No significant signal is observed for J/ψ→ μ+ μ− μ+ μ−, and an upper limit on the branching fraction is set at 1.6× 10− 6 at the 90% confidence level. A C P asymmetry observable is constructed for the first two channels, which is measured to be (− 0.012±0.054±0.010) and (0.062±0.059±0.006), respectively. No evidence for C P violation is observed in this process.

Euclid preparation. Measuring detailed galaxy morphologies for Euclid with Machine Learning

Authors

B Aussel,S Kruk,M Walmsley,M Huertas-Company,M Castellano,CJ Conselice,M Delli Veneri,H Domínguez Sánchez,P-A Duc,U Kuchner,A La Marca,B Margalef-Bentabol,FR Marleau,G Stevens,Y Toba,C Tortora,L Wang,N Aghanim,B Altieri,A Amara,S Andreon,N Auricchio,M Baldi,S Bardelli,R Bender,C Bodendorf,D Bonino,E Branchini,M Brescia,J Brinchmann,S Camera,V Capobianco,C Carbone,J Carretero,S Casas,S Cavuoti,A Cimatti,G Congedo,L Conversi,Y Copin,F Courbin,HM Courtois,M Cropper,A Da Silva,H Degaudenzi,AM Di Giorgio,J Dinis,F Dubath,X Dupac,S Dusini,M Farina,S Farrens,S Ferriol,S Fotopoulou,M Frailis,E Franceschi,P Franzetti,M Fumana,S Galeotta,B Garilli,B Gillis,C Giocoli,A Grazian,F Grupp,SVH Haugan,W Holmes,I Hook,F Hormuth,A Hornstrup,P Hudelot,K Jahnke,E Keihänen,S Kermiche,A Kiessling,M Kilbinger,B Kubik,M Kümmel,M Kunz,H Kurki-Suonio,R Laureijs,S Ligori,PB Lilje,V Lindholm,I Lloro,E Maiorano,O Mansutti,O Marggraf,K Markovic,N Martinet,F Marulli,R Massey,S Maurogordato,E Medinaceli,S Mei,Y Mellier,M Meneghetti,E Merlin,G Meylan,M Moresco,L Moscardini,E Munari,S-M Niemi,C Padilla,S Paltani,F Pasian,K Pedersen,WJ Percival,V Pettorino,S Pires,G Polenta,M Poncet,LA Popa,L Pozzetti,F Raison,R Rebolo,A Renzi,J Rhodes,G Riccio,E Romelli,M Roncarelli,E Rossetti,R Saglia,D Sapone,B Sartoris,M Schirmer,P Schneider,A Secroun,G Seidel,S Serrano,C Sirignano,G Sirri,L Stanco,J-L Starck,P Tallada-Crespí,AN Taylor,HI Teplitz,I Tereno,R Toledo-Moreo,F Torradeflot,I Tutusaus,EA Valentijn,L Valenziano,T Vassallo,A Veropalumbo,Y Wang,J Weller,A Zacchei,G Zamorani,J Zoubian,E Zucca

Journal

arXiv preprint arXiv:2402.10187

Published Date

2024/2/15

The Euclid mission is expected to image millions of galaxies with high resolution, providing an extensive dataset to study galaxy evolution. We investigate the application of deep learning to predict the detailed morphologies of galaxies in Euclid using Zoobot a convolutional neural network pretrained with 450000 galaxies from the Galaxy Zoo project. We adapted Zoobot for emulated Euclid images, generated based on Hubble Space Telescope COSMOS images, and with labels provided by volunteers in the Galaxy Zoo: Hubble project. We demonstrate that the trained Zoobot model successfully measures detailed morphology for emulated Euclid images. It effectively predicts whether a galaxy has features and identifies and characterises various features such as spiral arms, clumps, bars, disks, and central bulges. When compared to volunteer classifications Zoobot achieves mean vote fraction deviations of less than 12% and an accuracy above 91% for the confident volunteer classifications across most morphology types. However, the performance varies depending on the specific morphological class. For the global classes such as disk or smooth galaxies, the mean deviations are less than 10%, with only 1000 training galaxies necessary to reach this performance. For more detailed structures and complex tasks like detecting and counting spiral arms or clumps, the deviations are slightly higher, around 12% with 60000 galaxies used for training. In order to enhance the performance on complex morphologies, we anticipate that a larger pool of labelled galaxies is needed, which could be obtained using crowdsourcing. Finally, our findings imply …

Euclid preparation: TBD. The pre-launch Science Ground Segment simulation framework

Authors

S Serrano,P Hudelot,G Seidel,JE Pollack,E Jullo,F Torradeflot,D Benielli,R Fahed,T Auphan,J Carretero,H Aussel,P Casenove,FJ Castander,JE Davies,N Fourmanoit,S Huot,A Kara,E Keihanen,S Kermiche,K Okumura,J Zoubian,A Ealet,A Boucaud,H Bretonniere,R Casas,B Clement,CAJ Duncan,K George,K Kiiveri,H Kurki-Suonio,M Kummel,D Laugier,G Mainetti,JJ Mohr,A Montoro,C Neissner,M Schirmer,P Tallada-Crespi,N Tonello,A Venhola,A Verderi,A Zacchei,N Aghanim,B Altieri,A Amara,S Andreon,N Auricchio,R Azzollini,M Baldi,S Bardelli,A Basset,P Battaglia,C Bodendorf,D Bonino,E Branchini,M Brescia,J Brinchmann,S Camera,GP Candini,V Capobianco,C Carbone,S Casas,M Castellano,S Cavuoti,A Cimatti,R Cledassou,G Congedo,CJ Conselice,L Conversi,Y Copin,L Corcione,F Courbin,HM Courtois,M Cropper,A Da Silva,H Degaudenzi,AM Di Giorgio,J Dinis,F Dubath,X Dupac,S Dusini,M Farina,S Farrens,S Ferriol,M Frailis,E Franceschi,P Franzetti,S Galeotta,B Garilli,W Gillard,B Gillis,C Giocoli,BR Granett,A Grazian,F Grupp,L Guzzo,SVH Haugan,J Hoar,H Hoekstra,W Holmes,I Hook,F Hormuth,A Hornstrup,K Jahnke,B Joachimi,A Kiessling,T Kitching,R Kohley,M Kunz,Q Le Boulc'h,S Ligori,PB Lilje,V Lindholm,I Lloro,D Maino,E Maiorano,O Mansutti,O Marggraf,K Markovic,N Martinet,F Marulli,R Massey,S Maurogordato,E Medinaceli,S Mei,M Melchior,Y Mellier,M Meneghetti,E Merlin,G Meylan,M Moresco,L Moscardini,E Munari,R Nakajima,S-M Niemi,T Nutma,C Padilla,S Paltani,F Pasian,K Pedersen,WJ Percival,V Pettorino,S Pires,G Polenta,M Poncet,LA Popa,L Pozzetti,F Raison,R Rebolo,A Renzi

Journal

arXiv preprint arXiv:2401.01452

Published Date

2024/1/2

The European Space Agency's Euclid mission is one of the upcoming generation of large-scale cosmology surveys, which will map the large-scale structure in the Universe with unprecedented precision. The development and validation of the SGS pipeline requires state-of-the-art simulations with a high level of complexity and accuracy that include subtle instrumental features not accounted for previously as well as faster algorithms for the large-scale production of the expected Euclid data products. In this paper, we present the Euclid SGS simulation framework as applied in a large-scale end-to-end simulation exercise named Science Challenge 8. Our simulation pipeline enables the swift production of detailed image simulations for the construction and validation of the Euclid mission during its qualification phase and will serve as a reference throughout operations. Our end-to-end simulation framework starts with the production of a large cosmological N-body & mock galaxy catalogue simulation. We perform a selection of galaxies down to I_E=26 and 28 mag, respectively, for a Euclid Wide Survey spanning 165 deg^2 and a 1 deg^2 Euclid Deep Survey. We build realistic stellar density catalogues containing Milky Way-like stars down to H<26. Using the latest instrumental models for both the Euclid instruments and spacecraft as well as Euclid-like observing sequences, we emulate with high fidelity Euclid satellite imaging throughout the mission's lifetime. We present the SC8 data set consisting of overlapping visible and near-infrared Euclid Wide Survey and Euclid Deep Survey imaging and low-resolution spectroscopy along with ground-based …

Euclid: Testing photometric selection of emission-line galaxy targets

Authors

MS Cagliari,BR Granett,L Guzzo,M Bethermin,M Bolzonella,S de la Torre,P Monaco,M Moresco,WJ Percival,C Scarlata,Y Wang,M Ezziati,O Ilbert,V Le Brun,A Amara,S Andreon,N Auricchio,M Baldi,S Bardelli,R Bender,C Bodendorf,E Branchini,M Brescia,J Brinchmann,S Camera,V Capobianco,C Carbone,J Carretero,S Casas,M Castellano,S Cavuoti,A Cimatti,G Congedo,CJ Conselice,L Conversi,Y Copin,L Corcione,F Courbin,HM Courtois,A Da Silva,H Degaudenzi,AM Di Giorgio,J Dinis,F Dubath,CAJ Duncan,X Dupac,S Dusini,A Ealet,M Farina,S Farrens,S Ferriol,S Fotopoulou,M Frailis,E Franceschi,S Galeotta,B Gillis,C Giocoli,A Grazian,F Grupp,SVH Haugan,H Hoekstra,I Hook,F Hormuth,A Hornstrup,K Jahnke,E Keihänen,S Kermiche,A Kiessling,M Kilbinger,B Kubik,M Kümmel,M Kunz,H Kurki-Suonio,S Ligori,PB Lilje,V Lindholm,I Lloro,D Maino,E Maiorano,O Mansutti,O Marggraf,K Markovic,N Martinet,F Marulli,R Massey,S Maurogordato,HJ McCracken,E Medinaceli,S Mei,Y Mellier,M Meneghetti,E Merlin,G Meylan,L Moscardini,E Munari,RC Nichol,S-M Niemi,C Padilla,S Paltani,F Pasian,K Pedersen,V Pettorino,S Pires,G Polenta,M Poncet,LA Popa,L Pozzetti,F Raison,R Rebolo,A Renzi,J Rhodes,G Riccio,E Romelli,M Roncarelli,E Rossetti,R Saglia,D Sapone,B Sartoris,P Schneider,M Scodeggio,A Secroun,G Seidel,M Seiffert,S Serrano,C Sirignano,G Sirri,J Skottfelt,L Stanco,C Surace,AN Taylor,HI Teplitz,I Tereno,R Toledo-Moreo,F Torradeflot,I Tutusaus,EA Valentijn,L Valenziano,T Vassallo,A Veropalumbo,J Weller,G Zamorani,J Zoubian,E Zucca,C Burigana,V Scottez,M Viel,L Bisigello

Journal

arXiv preprint arXiv:2403.08726

Published Date

2024/3/13

Multi-object spectroscopic galaxy surveys typically make use of photometric and colour criteria to select targets. Conversely, the Euclid NISP slitless spectrograph will record spectra for every source over its field of view. Slitless spectroscopy has the advantage of avoiding defining a priori a galaxy sample, but at the price of making the selection function harder to quantify. The Euclid Wide Survey aims at building robust statistical samples of emission-line galaxies with fluxes in the Halpha-NII complex brighter than 2e-16 erg/s/cm^2 and within 0.9<z<1.8. At faint fluxes, we expect significant contamination by wrongly measured redshifts, either due to emission-line misidentification or noise fluctuations, with the consequence of reducing the purity of the final samples. This can be significantly improved by exploiting Euclid photometric information to identify emission-line galaxies over the redshifts of interest. To this goal, we compare and quantify the performance of six machine-learning classification algorithms. We consider the case when only Euclid photometric and morphological measurements are used and when these are supplemented by ground-based photometric data. We train and test the classifiers on two mock galaxy samples, the EL-COSMOS and Euclid Flagship2 catalogues. Dense neural networks and support vector classifiers obtain the best performance, with comparable results in terms of the adopted metrics. When training on Euclid photometry alone, these can remove 87% of the sources that are fainter than the nominal flux limit or lie outside the range 0.9<z<1.8, a figure that increases to 97% when ground-based photometry is …

Euclid: Identifying the reddest high-redshift galaxies in the Euclid Deep Fields with gradient-boosted trees

Authors

T Signor,G Rodighiero,L Bisigello,M Bolzonella,KI Caputi,E Daddi,G De Lucia,A Enia,L Gabarra,C Gruppioni,A Humphrey,F La Franca,C Mancini,L Pozzetti,S Serjeant,L Spinoglio,SE van Mierlo,S Andreon,N Auricchio,M Baldi,S Bardelli,P Battaglia,R Bender,C Bodendorf,D Bonino,E Branchini,M Brescia,J Brinchmann,S Camera,V Capobianco,C Carbone,J Carretero,S Casas,M Castellano,S Cavuoti,A Cimatti,R Cledassou,G Congedo,CJ Conselice,L Conversi,Y Copin,L Corcione,F Courbin,HM Courtois,A Da Silva,H Degaudenzi,AM Di Giorgio,J Dinis,F Dubath,X Dupac,S Dusini,A Ealet,M Farina,S Farrens,S Ferriol,S Fotopoulou,E Franceschi,S Galeotta,B Garilli,W Gillard,B Gillis,C Giocoli,A Grazian,F Grupp,L Guzzo,SVH Haugan,I Hook,F Hormuth,A Hornstrup,K Jahnke,M Kümmel,S Kermiche,A Kiessling,M Kilbinger,T Kitching,H Kurki-Suonio,S Ligori,PB Lilje,V Lindholm,I Lloro,D Maino,E Maiorano,O Mansutti,O Marggraf,N Martinet,F Marulli,R Massey,E Medinaceli,M Melchior,Y Mellier,M Meneghetti,E Merlin,M Moresco,L Moscardini,E Munari,RC Nichol,S-M Niemi,C Padilla,S Paltani,F Pasian,K Pedersen,V Pettorino,S Pires,G Polenta,M Poncet,LA Popa,F Raison,A Renzi,J Rhodes,G Riccio,E Romelli,M Roncarelli,E Rossetti,R Saglia,D Sapone,B Sartoris,P Schneider,T Schrabback,A Secroun,G Seidel,S Serrano,C Sirignano,G Sirri,L Stanco,C Surace,P Tallada-Crespí,HI Teplitz,I Tereno,R Toledo-Moreo,F Torradeflot,I Tutusaus,EA Valentijn,T Vassallo,A Veropalumbo,Y Wang,J Weller,OR Williams,J Zoubian,E Zucca,C Burigana,V Scottez,Euclid Collaboration

Journal

arXiv preprint arXiv:2402.04800

Published Date

2024/2/7

Dusty, distant, massive () galaxies are usually found to show a remarkable star-formation activity, contributing on the order of of the cosmic star-formation rate density at --, and up to at from ALMA observations. Nonetheless, they are elusive in classical optical surveys, and current near-infrared surveys are able to detect them only in very small sky areas. Since these objects have low space densities, deep and wide surveys are necessary to obtain statistically relevant results about them. Euclid will be potentially capable of delivering the required information, but, given the lack of spectroscopic features at these distances within its bands, it is still unclear if it will be possible to identify and characterize these objects. The goal of this work is to assess the capability of Euclid, together with ancillary optical and near-infrared data, to identify these distant, dusty and massive galaxies, based on broadband photometry. We used a gradient-boosting algorithm to predict both the redshift and spectral type of objects at high . To perform such an analysis we make use of simulated photometric observations derived using the SPRITZ software. The gradient-boosting algorithm was found to be accurate in predicting both the redshift and spectral type of objects within the Euclid Deep Survey simulated catalog at . In particular, we study the analog of HIEROs (i.e. sources with ), combining Euclid and Spitzer data at the depth of the Deep Fields. We found that the dusty population at is well identified, with a redshift RMS and OLF of only and (), respectively. Our findings suggest that with Euclid we …

Euclid preparation-XXXII. Evaluating the weak-lensing cluster mass biases using the Three Hundred Project hydrodynamical simulations

Authors

C Giocoli,M Meneghetti,E Rasia,S Borgani,G Despali,GF Lesci,F Marulli,L Moscardini,M Sereno,W Cui,A Knebe,G Yepes,T Castro,P-S Corasaniti,S Pires,G Castignani,T Schrabback,GW Pratt,AMC Le Brun,N Aghanim,L Amendola,N Auricchio,M Baldi,C Bodendorf,D Bonino,E Branchini,M Brescia,J Brinchmann,S Camera,V Capobianco,C Carbone,J Carretero,FJ Castander,M Castellano,S Cavuoti,R Cledassou,G Congedo,CJ Conselice,L Conversi,Y Copin,L Corcione,F Courbin,M Cropper,A Da Silva,H Degaudenzi,J Dinis,F Dubath,X Dupac,S Dusini,S Farrens,S Ferriol,P Fosalba,M Frailis,E Franceschi,M Fumana,S Galeotta,B Garilli,B Gillis,A Grazian,F Grupp,SVH Haugan,W Holmes,A Hornstrup,K Jahnke,M Kümmel,S Kermiche,M Kilbinger,M Kunz,H Kurki-Suonio,S Ligori,PB Lilje,I Lloro,E Maiorano,O Mansutti,O Marggraf,K Markovic,R Massey,S Maurogordato,S Mei,E Merlin,G Meylan,M Moresco,E Munari,S-M Niemi,J Nightingale,T Nutma,C Padilla,S Paltani,F Pasian,K Pedersen,V Pettorino,G Polenta,M Poncet,LA Popa,F Raison,A Renzi,J Rhodes,G Riccio,E Romelli,M Roncarelli,E Rossetti,R Saglia,D Sapone,B Sartoris,P Schneider,A Secroun,S Serrano,C Sirignano,G Sirri,L Stanco,J-L Starck,P Tallada-Crespí,AN Taylor,I Tereno,R Toledo-Moreo,F Torradeflot,I Tutusaus,EA Valentijn,L Valenziano,T Vassallo,Y Wang,J Weller,G Zamorani,J Zoubian,S Andreon,S Bardelli,A Boucaud,E Bozzo,C Colodro-Conde,D Di Ferdinando,G Fabbian,M Farina,H Israel,E Keihänen,V Lindholm,N Mauri,C Neissner,M Schirmer,V Scottez,M Tenti,E Zucca,Y Akrami,C Baccigalupi,M Ballardini,F Bernardeau,A Biviano,AS Borlaff,C Burigana,R Cabanac,A Cappi

Journal

Astronomy & Astrophysics

Published Date

2024/1/1

The photometric catalogue of galaxy clusters extracted from ESA Euclid data is expected to be very competitive for cosmological studies. Using dedicated hydrodynamical simulations, we present systematic analyses simulating the expected weak-lensing profiles from clusters in a variety of dynamic states and for a wide range of redshifts. In order to derive cluster masses, we use a model consistent with the implementation within the Euclid Consortium of the dedicated processing function and find that when we jointly model the mass and concentration parameter of the Navarro–Frenk–White halo profile, the weak-lensing masses tend to be biased low by 5–10% on average with respect to the true mass, up to z = 0.5. For a fixed value for the concentration c200 = 3, the mass bias is decreases to lower than 5%, up to z = 0.7, along with the relative uncertainty. Simulating the weak-lensing signal by projecting …

Euclid preparation. Optical emission-line predictions of intermediate-z galaxy populations in GAEA for the Euclid Deep and Wide Surveys

Authors

L Scharré,M Hirschmann,G De Lucia,S Charlot,F Fontanot,M Spinelli,L Xie,A Feltre,V Allevato,A Plat,MN Bremer,S Fotopoulou,L Gabarra,BR Granett,M Moresco,C Scarlata,L Pozzetti,L Spinoglio,M Talia,G Zamorani,B Altieri,A Amara,S Andreon,N Auricchio,M Baldi,S Bardelli,D Bonino,E Branchini,M Brescia,J Brinchmann,S Camera,V Capobianco,C Carbone,J Carretero,S Casas,FJ Castander,M Castellano,S Cavuoti,A Cimatti,G Congedo,CJ Conselice,L Conversi,Y Copin,L Corcione,F Courbin,HM Courtois,A Da Silva,H Degaudenzi,J Dinis,M Douspis,F Dubath,X Dupac,S Dusini,M Farina,S Farrens,S Ferriol,M Frailis,E Franceschi,S Galeotta,B Garilli,B Gillis,C Giocoli,A Grazian,F Grupp,L Guzzo,SVH Haugan,W Holmes,I Hook,F Hormuth,A Hornstrup,K Jahnke,E Keihänen,S Kermiche,A Kiessling,T Kitching,B Kubik,M Kümmel,M Kunz,H Kurki-Suonio,S Ligori,PB Lilje,V Lindholm,I Lloro,D Maino,E Maiorano,O Mansutti,O Marggraf,K Markovic,N Martinet,F Marulli,R Massey,S Maurogordato,HJ McCracken,E Medinaceli,S Mei,Y Mellier,M Meneghetti,E Merlin,G Meylan,L Moscardini,E Munari,S-M Niemi,C Padilla,S Paltani,F Pasian,K Pedersen,V Pettorino,G Polenta,M Poncet,LA Popa,F Raison,A Renzi,J Rhodes,G Riccio,E Romelli,M Roncarelli,E Rossetti,R Saglia,D Sapone,B Sartoris,M Schirmer,P Schneider,A Secroun,G Seidel,S Serrano,C Sirignano,G Sirri,L Stanco,C Surace,P Tallada-Crespí,AN Taylor,HI Teplitz,I Tereno,R Toledo-Moreo,F Torradeflot,I Tutusaus,L Valenziano,T Vassallo,A Veropalumbo,Y Wang,J Weller,J Zoubian,E Zucca,A Biviano,M Bolzonella,E Bozzo,C Burigana,C Colodro-Conde,D Di Ferdinando,R Farinelli

Journal

arXiv preprint arXiv:2402.03436

Published Date

2024/2/5

In anticipation of the Euclid Wide and Deep Surveys, we present optical emission-line predictions at intermediate redshifts from 0.4 to 2.5. Our approach combines a mock light cone from the GAEA semi-analytic model to self-consistently model nebular emission from HII regions, narrow-line regions of active galactic nuclei (AGN), and evolved stellar populations. Our analysis focuses on seven optical emission lines: H, H, [SII], [NII], [OI], [OIII], and [OII]. We find that Euclid will predominantly observe massive, star-forming, and metal-rich line-emitters. Interstellar dust, modelled using a Calzetti law with mass-dependent scaling, may decrease observable percentages by a further 20-30% with respect to our underlying emission-line populations from GAEA. We predict Euclid to observe around 30-70% of H-, [NII]-, [SII]-, and [OIII]-emitting galaxies at redshift below 1 and under 10% at higher redshift. Observability of H-, [OII]-, and [OI]- emission is limited to below 5%. For the Euclid-observable sample, we find that BPT diagrams can effectively distinguish between different galaxy types up to around redshift 1.8, attributed to the bias toward metal-rich systems. Moreover, we show that the relationships of H and [OIII]+H to the star-formation rate, and the [OIII]-AGN luminosity relation, exhibit minimal changes with increasing redshift. Based on line ratios [NII]/H, [NII]/[OII], and [NII]/[SII], we further propose novel z-invariant tracers for the black hole accretion rate-to-star formation rate ratio. Lastly, we find that commonly used metallicity estimators display gradual shifts in normalisations with increasing redshift, while …

Euclid preparation-XXXI. The effect of the variations in photometric passbands on photometric-redshift accuracy

Authors

Stéphane Paltani,J Coupon,WG Hartley,A Alvarez-Ayllon,F Dubath,JJ Mohr,M Schirmer,J-C Cuillandre,G Desprez,O Ilbert,K Kuijken,N Aghanim,B Altieri,A Amara,N Auricchio,M Baldi,R Bender,C Bodendorf,D Bonino,E Branchini,M Brescia,J Brinchmann,S Camera,V Capobianco,C Carbone,VF Cardone,J Carretero,FJ Castander,M Castellano,S Cavuoti,R Cledassou,G Congedo,CJ Conselice,L Conversi,Y Copin,L Corcione,F Courbin,M Cropper,A Da Silva,H Degaudenzi,J Dinis,M Douspis,X Dupac,S Dusini,S Farrens,S Ferriol,P Fosalba,M Frailis,E Franceschi,P Franzetti,S Galeotta,B Garilli,W Gillard,B Gillis,C Giocoli,A Grazian,SV Haugan,H Hoekstra,A Hornstrup,P Hudelot,K Jahnke,M Kümmel,S Kermiche,A Kiessling,M Kilbinger,T Kitching,R Kohley,B Kubik,M Kunz,H Kurki-Suonio,S Ligori,PB Lilje,I Lloro,E Maiorano,O Mansutti,O Marggraf,K Markovic,F Marulli,R Massey,DC Masters,S Maurogordato,HJ Mccracken,E Medinaceli,S Mei,M Melchior,M Meneghetti,E Merlin,G Meylan,M Moresco,L Moscardini,E Munari,S-M Niemi,J Nightingale,C Padilla,F Pasian,K Pedersen,WJ Percival,V Pettorino,G Polenta,M Poncet,LA Popa,F Raison,R Rebolo,A Renzi,J Rhodes,G Riccio,E Romelli,M Roncarelli,E Rossetti,R Saglia,D Sapone,B Sartoris,P Schneider,A Secroun,C Sirignano,G Sirri,J Skottfelt,L Stanco,J-L Starck,C Surace,P Tallada-Crespí,I Tereno,R Toledo-Moreo,F Torradeflot,I Tutusaus,EA Valentijn,L Valenziano,T Vassallo,Y Wang,G Zamorani,J Zoubian,S Andreon,H Aussel,S Bardelli,M Bolzonella,A Boucaud,D Di Ferdinando,M Farina,J Graciá-Carpio,V Lindholm,D Maino,N Mauri,C Neissner,V Scottez,E Zucca,C Baccigalupi,M Ballardini,A Biviano,A Blanchard,S Borgani

Journal

Astronomy & Astrophysics

Published Date

2024/1/1

Euclid preparation. Improving cosmological constraints using a new multi-tracer method with the spectroscopic and photometric samples

Authors

Fabien Dournac,Alain Blanchard,Stéphane Ilić,Brahim Lamine,I Tutusaus,A Amara,S Andreon,N Auricchio,H Aussel,M Baldi,S Bardelli,C Bodendorf,D Bonino,E Branchini,Sylvie Brau-Nogue,M Brescia,J Brinchmann,S Camera,V Capobianco,J Carretero,S Casas,M Castellano,S Cavuoti,A Cimatti,G Congedo,CJ Conselice,L Conversi,Y Copin,F Courbin,HM Courtois,A Da Silva,H Degaudenzi,AM Di Giorgio,J Dinis,M Douspis,F Dubath,X Dupac,S Dusini,A Ealet,M Farina,S Farrens,S Ferriol,M Frailis,E Franceschi,S Galeotta,W Gillard,B Gillis,C Giocoli,BR Granett,A Grazian,F Grupp,SVH Haugan,W Holmes,I Hook,F Hormuth,A Hornstrup,P Hudelot,K Jahnke,E Keihänen,S Kermiche,A Kiessling,M Kilbinger,B Kubik,M Kümmel,M Kunz,H Kurki-Suonio,S Ligori,PB Lilje,V Lindholm,I Lloro,D Maino,E Maiorano,O Mansutti,O Marggraf,K Markovic,N Martinet,F Marulli,R Massey,S Maurogordato,E Medinaceli,S Mei,Y Mellier,M Meneghetti,E Merlin,G Meylan,M Moresco,L Moscardini,E Munari,S-M Niemi,JW Nightingale,C Padilla,S Paltani,F Pasian,K Pedersen,WJ Percival,V Pettorino,S Pires,G Polenta,M Poncet,LA Popa,L Pozzetti,F Raison,R Rebolo,A Renzi,J Rhodes,G Riccio,E Romelli,M Roncarelli,E Rossetti,R Saglia,D Sapone,P Schneider,A Secroun,G Seidel,M Seiffert,S Serrano,C Sirignano,G Sirri,L Stanco,C Surace,P Tallada-Crespí,D Tavagnacco,AN Taylor,I Tereno,R Toledo-Moreo,F Torradeflot,EA Valentijn,L Valenziano,T Vassallo,A Veropalumbo,Y Wang,A Zacchei,G Zamorani,J Zoubian,E Zucca,A Biviano,M Bolzonella,A Boucaud,E Bozzo,C Burigana,C Colodro-Conde,G De Lucia,D Di Ferdinando,JA Vigo,R Farinelli,J Gracia-Carpio,G Mainetti,M Martinelli,N Mauri,C Neissner

Journal

arXiv preprint arXiv:2404.12157

Published Date

2024/4/18

Future data provided by the \Euclid mission will allow us to better understand the cosmic history of the Universe. A metric of its performance is the figure-of-merit (FoM) of dark energy, usually estimated with Fisher forecasts. The expected FoM has previously been estimated taking into account the two main probes of \Euclid, namely the three-dimensional clustering of the spectroscopic galaxy sample, and the so-called 32\,pt signal from the photometric sample (i.e., the weak lensing signal, the galaxy clustering, and their cross-correlation). So far, these two probes have been treated as independent. In this paper, we introduce a new observable given by the ratio of the (angular) two-point correlation function of galaxies from the two surveys. For identical (normalised) selection functions, this observable is unaffected by sampling noise, and its variance is solely controlled by Poisson noise. We present forecasts for \Euclid where this multi-tracer method is applied and is particularly relevant because the two surveys will cover the same area of the sky. This method allows for the exploitation of the combination of the spectroscopic and photometric samples. When the correlation between this new observable and the other probes is not taken into account, a significant gain is obtained in the FoM, as well as in the constraints on other cosmological parameters. The benefit is more pronounced for a commonly investigated modified gravity model, namely the parametrisation of the growth factor. However, the correlation between the different probes is found to be significant and hence the actual gain is uncertain. We present various strategies for …

Measurement of branching fraction of relative to

Authors

M Ablikim,MN Achasov,P Adlarson,M Albrecht,R Aliberti,A Amoroso,MR An,Q An,XH Bai,Y Bai,O Bakina,R Baldini Ferroli,I Balossino,Y Ban,V Batozskaya,D Becker,K Begzsuren,N Berger,M Bertani,D Bettoni,F Bianchi,J Bloms,A Bortone,I Boyko,RA Briere,A Brueggemann,H Cai,X Cai,A Calcaterra,GF Cao,N Cao,SA Cetin,JF Chang,WL Chang,Chao Chen,Chao Chen,G Chen,HS Chen,ML Chen,SJ Chen,SM Chen,T Chen,XR Chen,XT Chen,YB Chen,ZJ Chen,WS Cheng,SK Choi,X Chu,G Cibinetto,F Cossio,JJ Cui,HL Dai,JP Dai,A Dbeyssi,RE de Boer,D Dedovich,ZY Deng,A Denig,I Denysenko,M Destefanis,F De Mori,Y Ding,J Dong,LY Dong,MY Dong,X Dong,SX Du,P Egorov,YL Fan,J Fang,SS Fang,WX Fang,Y Fang,R Farinelli,L Fava,F Feldbauer,G Felici,CQ Feng,JH Feng,K Fischer,M Fritsch,C Fritzsch,CD Fu,H Gao,YN Gao,Yang Gao,S Garbolino,I Garzia,PT Ge,ZW Ge,C Geng,EM Gersabeck,A Gilman,K Goetzen,L Gong,WX Gong,W Gradl,M Greco,LM Gu,MH Gu,YT Gu,CY Guan,AQ Guo,LB Guo,RP Guo,YP Guo,A Guskov,TT Han,WY Han,XQ Hao,FA Harris,KK He,KL He,FH Heinsius,CH Heinz,YK Heng,C Herold,GY Hou,YR Hou,ZL Hou,HM Hu,JF Hu,T Hu,Y Hu,GS Huang,KX Huang,LQ Huang,XT Huang,YP Huang,Z Huang,T Hussain,N Hüsken,W Imoehl,M Irshad,J Jackson,S Jaeger,S Janchiv,E Jang,JH Jeong,Q Ji,QP Ji,XB Ji,XL Ji,YY Ji,ZK Jia,HB Jiang,SS Jiang,XS Jiang,Y Jiang

Journal

Physical Review D

Published Date

2023/2/27

Based on 7.33 fb− 1 of e+ e− collision data taken at center-of-mass energies between 4.128 and 4.226 GeV with the BESIII detector, we measure the branching fraction of D s*+→ D s+ π 0 relative to that of D s*+→ D s+ γ to be (6.16±0.43±0.18)%. The first uncertainty is statistical and the second one is systematic. By using the world average value of the branching fraction of D s*+→ D s+ e+ e−, we determine the branching fractions of D s*+→ D s+ γ and D s*+→ D s+ π 0 to be (93.57±0.38±0.22)% and (5.76±0.38±0.16)%, respectively.

Evidence for the decay

Authors

M Ablikim,MN Achasov,P Adlarson,M Albrecht,R Aliberti,A Amoroso,MR An,Q An,Y Bai,O Bakina,R Baldini Ferroli,I Balossino,Y Ban,V Batozskaya,D Becker,K Begzsuren,N Berger,M Bertani,D Bettoni,F Bianchi,E Bianco,J Bloms,A Bortone,I Boyko,RA Briere,A Brueggemann,H Cai,X Cai,A Calcaterra,GF Cao,N Cao,SA Cetin,JF Chang,WL Chang,GR Che,Chao Chen,Chao Chen,G Chen,HS Chen,ML Chen,SJ Chen,SM Chen,T Chen,XR Chen,XT Chen,YB Chen,ZJ Chen,WS Cheng,SK Choi,X Chu,G Cibinetto,F Cossio,JJ Cui,HL Dai,JP Dai,A Dbeyssi,RE de Boer,D Dedovich,ZY Deng,A Denig,I Denysenko,M Destefanis,F De Mori,Y Ding,J Dong,LY Dong,MY Dong,X Dong,SX Du,ZH Duan,P Egorov,YL Fan,J Fang,SS Fang,WX Fang,Y Fang,R Farinelli,L Fava,F Feldbauer,G Felici,CQ Feng,JH Feng,K Fischer,M Fritsch,C Fritzsch,CD Fu,H Gao,YN Gao,Yang Gao,S Garbolino,I Garzia,PT Ge,ZW Ge,C Geng,EM Gersabeck,A Gilman,K Goetzen,L Gong,WX Gong,W Gradl,M Greco,LM Gu,MH Gu,YT Gu,CY Guan,AQ Guo,LB Guo,RP Guo,YP Guo,A Guskov,WY Han,XQ Hao,FA Harris,KK He,KL He,FH Heinsius,CH Heinz,YK Heng,C Herold,GY Hou,YR Hou,ZL Hou,HM Hu,JF Hu,T Hu,Y Hu,GS Huang,KX Huang,LQ Huang,XT Huang,YP Huang,Z Huang,T Hussain,N Hüsken,W Imoehl,M Irshad,J Jackson,S Jaeger,S Janchiv,E Jang,JH Jeong,Q Ji,QP Ji,XB Ji,XL Ji,YY Ji,ZK Jia,SS Jiang,XS Jiang,Y Jiang

Journal

Physical Review D

Published Date

2023/3/17

The decay η c (2 S)→ π+ π− η is searched for through the radiative transition ψ (3686)→ γ η c (2 S) using 448 million ψ (3686) events accumulated at the BESIII detector. The first evidence of η c (2 S)→ π+ π− η is found with a statistical significance of 3.5 σ. The product of the branching fractions of ψ (3686)→ γ η c (2 S) and η c (2 S)→ π+ π− η is measured to be Br (ψ (3686)→ γ η c (2 S))× Br (η c (2 S)→ π+ π− η)=(2.97±0.81±0.26)× 10− 6, where the first uncertainty is statistical and the second one is systematic. The branching fraction of the decay η c (2 S)→ π+ π− η is determined to be Br (η c (2 S)→ π+ π− η)=(42.4±11.6±3.8±30.3)× 10− 4, where the third uncertainty is transferred from the uncertainty of the branching fraction of ψ (3686)→ γ η c (2 S).

Measurement of from 3.5106 to 4.6988 GeV and study of mass threshold enhancement

Authors

Wei Xu,M Ablikim,MN Achasov,P Adlarson,M Albrecht,R Aliberti,A Amoroso,MR An,Q An,Y Bai,O Bakina,R Baldini Ferroli,I Balossino,Y Ban,V Batozskaya,D Becker,K Begzsuren,N Berger,M Bertani,D Bettoni,F Bianchi,E Bianco,J Bloms,A Bortone,I Boyko,RA Briere,A Brueggemann,H Cai,X Cai,A Calcaterra,GF Cao,N Cao,SA Cetin,JF Chang,WL Chang,GR Che,Chao Chen,Chao Chen,G Chen,HS Chen,ML Chen,SJ Chen,SM Chen,T Chen,XR Chen,XT Chen,YB Chen,ZJ Chen,WS Cheng,SK Choi,X Chu,G Cibinetto,F Cossio,JJ Cui,HL Dai,JP Dai,A Dbeyssi,RE de Boer,D Dedovich,ZY Deng,A Denig,I Denysenko,M Destefanis,F De Mori,Y Ding,J Dong,LY Dong,MY Dong,X Dong,SX Du,ZH Duan,P Egorov,YL Fan,J Fang,SS Fang,WX Fang,Y Fang,R Farinelli,L Fava,F Feldbauer,G Felici,CQ Feng,JH Feng,K Fischer,M Fritsch,C Fritzsch,CD Fu,H Gao,YN Gao,Yang Gao,S Garbolino,I Garzia,PT Ge,ZW Ge,C Geng,EM Gersabeck,A Gilman,K Goetzen,L Gong,WX Gong,W Gradl,M Greco,LM Gu,MH Gu,YT Gu,CY Guan,AQ Guo,LB Guo,RP Guo,YP Guo,A Guskov,WY Han,XQ Hao,FA Harris,KK He,KL He,FH Heinsius,CH Heinz,YK Heng,C Herold,GY Hou,YR Hou,ZL Hou,HM Hu,JF Hu,T Hu,Y Hu,GS Huang,KX Huang,LQ Huang,XT Huang,YP Huang,Z Huang,T Hussain,N Hüsken,W Imoehl,M Irshad,J Jackson,S Jaeger,S Janchiv,E Jang,JH Jeong,Q Ji,QP Ji,XB Ji,XL Ji,YY Ji,ZK Jia,PC Jiang,SS Jiang

Journal

Physical Review D

Published Date

2023/6/1

Using data samples with a total integrated luminosity of approximately 18 fb− 1 collected by the BESIII detector operating at the Beijing Electron-Positron Collider II, the process e+ e−→ Λ Λη is studied at center-of-mass energies between 3.5106 and 4.6988 GeV. The Born cross section for the process e+ e−→ Λ Λη is measured. No significant structure is observed in the Born cross section line shape. An enhancement near the Λ Λmass threshold is observed for the first time in the process. The structure can be described by an S-wave Breit-Wigner function. Neglecting contribution of excited Λ states and potential interferences, the mass and width are determined to be (2356±7±15) MeV/c 2 and (304±28±54) MeV, respectively, where the first uncertainties are statistical and the second are systematic.

Observation of the and evidence for a new vector charmoniumlike state in

Authors

Journal

Physical Review D

Published Date

2023/5/8

Cross sections for the process e+ e−→ K S 0 K S 0 J/ψ at center-of-mass energies from 4.128 to 4.950 GeV are measured using data samples with a total integrated luminosity of 21.2 fb− 1 collected by the BESIII detector operating at the BEPCII storage ring. The Y (4230) state is observed in the energy dependence of the e+ e−→ K S 0 K S 0 J/ψ cross section for the first time with a statistical significance of 26.0 σ. In addition, an enhancement around 4.710 GeV, labeled as the Y (4710), is seen with a statistical significance of 4.2 σ. There is no clear structure around 4.484 GeV. Using a fit with a coherent sum of three Breit-Wigner functions, we determine the mass and width of the Y (4230) state to be 4226.9±6.6±22.0 MeV/c 2 and 71.7±16.2±32.8 MeV, respectively, and the mass and width of the Y (4710) state to be 4704.0±52.3±69.5 MeV/c 2 and 183.2±114.0±96.1 MeV, respectively, where the first uncertainties are …

Novel method to extract the femtometer structure of strange baryons using the vacuum polarization effect

Authors

M Ablikim,MN Achasov,P Adlarson,M Albrecht,R Aliberti,A Amoroso,MR An,Q An,Y Bai,O Bakina,R Baldini Ferroli,I Balossino,Y Ban,V Batozskaya,D Becker,K Begzsuren,N Berger,M Bertani,D Bettoni,F Bianchi,E Bianco,J Bloms,A Bortone,I Boyko,RA Briere,A Brueggemann,H Cai,X Cai,A Calcaterra,GF Cao,N Cao,SA Cetin,JF Chang,WL Chang,GR Che,C Chen,Chao Chen,G Chen,HS Chen,ML Chen,SJ Chen,SM Chen,T Chen,XR Chen,XT Chen,YB Chen,ZJ Chen,WS Cheng,SK Choi,X Chu,G Cibinetto,F Cossio,JJ Cui,HL Dai,JP Dai,A Dbeyssi,RE de Boer,D Dedovich,ZY Deng,A Denig,I Denysenko,M Destefanis,F De Mori,Y Ding,J Dong,LY Dong,MY Dong,X Dong,SX Du,ZH Duan,P Egorov,YL Fan,J Fang,SS Fang,WX Fang,Y Fang,R Farinelli,L Fava,F Feldbauer,G Felici,CQ Feng,JH Feng,K Fischer,M Fritsch,C Fritzsch,CD Fu,H Gao,YN Gao,Yang Gao,S Garbolino,I Garzia,PT Ge,ZW Ge,C Geng,EM Gersabeck,A Gilman,K Goetzen,L Gong,WX Gong,W Gradl,M Greco,LM Gu,MH Gu,YT Gu,CY Guan,AQ Guo,LB Guo,RP Guo,YP Guo,A Guskov,WY Han,XQ Hao,FA Harris,KK He,KL He,FH Heinsius,CH Heinz,YK Heng,C Herold,GY Hou,YR Hou,ZL Hou,HM Hu,JF Hu,T Hu,Y Hu,GS Huang,KX Huang,LQ Huang,XT Huang,YP Huang,Z Huang,T Hussain,N Hüsken,W Imoehl,M Irshad,J Jackson,S Jaeger,S Janchiv,E Jang,JH Jeong,Q Ji,QP Ji,XB Ji,XL Ji,YY Ji,ZK Jia,PC Jiang,SS Jiang,XS Jiang

Journal

arXiv preprint arXiv:2309.04139

Published Date

2023/9/8

One of the fundamental goals of particle physics is to gain microscopic understanding of the strong interaction. Electromagnetic form factors quantify the structure of hadrons in terms of charge and magnetization distributions. While the nucleon structure has been investigated extensively, data on hyperons is still scarce. It has recently been demonstrated that electron-positron annihilations into hyperon-antihyperon pairs provide a powerful tools to investigate their inner structure. We present a novel method useful for hyperon-antihyperon pairs of different types which exploits the cross section enhancement due to the vacuum polarization effect at the resonance. Using the 10 billion events collected with the BESIII detector, this allows a thorough determination of the hyperon structure . The result is essentially a precise snapshot of a ~() pair in the making, encoded in the form factor ratio and the phase. Their values are measured to be , $\Delta\Phi_1=(1.011\pm0.094({\rm stat.})\pm0.010({\rm syst.}))~\rm rad$ for and $\Delta\Phi_2=(2.128\pm0.094({\rm stat.})\pm0.010({\rm syst.}))~\rm rad$ for , respectively. Furthermore, charge-parity (CP) breaking is investigated for the first time in this reaction and found to be consistent with CP symmetry.

Euclid preparation-XXX. Performance assessment of the NISP red grism through spectroscopic simulations for the wide and deep surveys

Authors

Louis Gabarra,C Mancini,L Rodriguez Muñoz,G Rodighiero,C Sirignano,M Scodeggio,M Talia,S Dusini,W Gillard,BR Granett,E Maiorano,M Moresco,L Paganin,E Palazzi,L Pozzetti,A Renzi,E Rossetti,D Vergani,V Allevato,L Bisigello,G Castignani,B De Caro,M Fumana,K Ganga,B Garilli,M Hirschmann,F La Franca,C Laigle,F Passalacqua,M Schirmer,L Stanco,A Troja,LYA Yung,G Zamorani,J Zoubian,S Anselmi,F Oppizzi,G Verza,N Aghanim,A Amara,N Auricchio,M Baldi,R Bender,C Bodendorf,D Bonino,E Branchini,Massimo Brescia,J Brinchmann,S Camera,V Capobianco,C Carbone,J Carretero,FJ Castander,M Castellano,Stefano Cavuoti,R Cledassou,G Congedo,CJ Conselice,L Conversi,Y Copin,L Corcione,A Costille,F Courbin,A Da Silva,H Degaudenzi,J Dinis,F Dubath,X Dupac,A Ealet,S Farrens,S Ferriol,M Frailis,E Franceschi,P Franzetti,S Galeotta,B Gillis,C Giocoli,A Grazian,F Grupp,L Guzzo,W Holmes,A Hornstrup,P Hudelot,K Jahnke,M Kümmel,S Kermiche,A Kiessling,M Kilbinger,T Kitching,R Kohley,B Kubik,M Kunz,Hannu Kurki-Suonio,S Ligori,Per Barth Lilje,I Lloro,O Mansutti,O Marggraf,K Markovic,F Marulli,Richard Massey,S Maurogordato,S Mei,M Meneghetti,G Meylan,L Moscardini,E Munari,RC Nichol,S-M Niemi,J Nightingale,C Padilla,S Paltani,F Pasian,K Pedersen,WJ Percival,V Pettorino,G Polenta,M Poncet,F Raison,J Rhodes,G Riccio,E Romelli,M Roncarelli,R Saglia,D Sapone,P Schneider,A Secroun,G Seidel,S Serrano,G Sirri,C Surace,P Tallada-Crespí,D Tavagnacco,AN Taylor,I Tereno,R Toledo-Moreo,F Torradeflot,M Trifoglio,I Tutusaus,EA Valentijn,L Valenziano,T Vassallo,Y Wang,J Weller,A Zacchei,S Andreon,H Aussel,S Bardelli,M Bolzonella,A Boucaud

Journal

Astronomy & Astrophysics

Published Date

2023/8/1

This work focusses on the pilot run of a simulation campaign aimed at investigating the spectroscopic capabilities of the Euclid Near-Infrared Spectrometer and Photometer (NISP), in terms of continuum and emission line detection in the context of galaxy evolutionary studies. To this purpose, we constructed, emulated, and analysed the spectra of 4992 star-forming galaxies at 0.3 ≤ z ≤ 2.5 using the NISP pixel-level simulator. We built the spectral library starting from public multi-wavelength galaxy catalogues, with value-added information on spectral energy distribution (SED) fitting results, and stellar population templates from Bruzual & Charlot (2003, MNRAS, 344, 1000). Rest-frame optical and near-IR nebular emission lines were included using empirical and theoretical relations. Dust attenuation was treated using the Calzetti extinction law accounting for the differential attenuation in line-emitting regions with …

See List of Professors in Miriam Kümmel University(Ruhr-Universität Bochum)

Miriam Kümmel FAQs

What is Miriam Kümmel's h-index at Ruhr-Universität Bochum?

The h-index of Miriam Kümmel has been 41 since 2020 and 48 in total.

What are Miriam Kümmel's top articles?

The articles with the titles of

Euclid: Validation of the MontePython forecasting tools

Euclid preparation-XXXIII. Characterization of convolutional neural networks for the identification of galaxy-galaxy strong-lensing events

Euclid preparation-XXXVII. Galaxy colour selections with Euclid and ground photometry for cluster weak-lensing analyses

Euclid preparation

Euclid preparation-XXXV. Covariance model validation for the two-point correlation function of galaxy clusters

Observation of decays to and

Euclid preparation. Measuring detailed galaxy morphologies for Euclid with Machine Learning

Euclid preparation: TBD. The pre-launch Science Ground Segment simulation framework

...

are the top articles of Miriam Kümmel at Ruhr-Universität Bochum.

What are Miriam Kümmel's research interests?

The research interests of Miriam Kümmel are: hadron physics

What is Miriam Kümmel's total number of citations?

Miriam Kümmel has 9,503 citations in total.

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