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171 results on '"W. Van Driel"'

1. Searching in H i for Massive Low Surface Brightness Galaxies: Samples from HyperLeda and the UGC

Author

K. O’Neil, Stephen E. Schneider, W. van Driel, G. Liu, T. Joseph, A. C. Schwortz, and Z. Butcher

Subjects
Amorphous irregular galaxies, Radio astronomy, Spiral galaxies, Low surface brightness galaxies, Astronomy, QB1-991
Abstract

A search has been made for 21 cm H i line emission in a total of 350 unique galaxies from two samples whose optical properties indicate they may be massive. The first consists of 241 low surface brightness (LSB) galaxies of morphological type Sb and later selected from the HyperLeda database and the second consists of 119 LSB galaxies from the UGC with morphological types Sd-m and later. Of the 350 unique galaxies, 239 were observed at the Nançay Radio Telescope, 161 at the Green Bank Telescope, and 66 at the Arecibo telescope. A total of 295 (84.3%) were detected, of which 253 (72.3%) appear to be uncontaminated by any other galaxies within the telescope beam. Finally, of the total detected, uncontaminated galaxies, at least 31 appear to be massive LSB galaxies, with a total H i mass ≥ 10 ^10 M _⊙ , for H _0 = 70 kms ^−1 Mpc ^−1 . If we expand the definition to also include galaxies with significant total (rather than just gas) mass, i.e., those with an inclination-corrected H i line width W _50,cor > 500 km s ^−1 , this brings the total number of massive LSB galaxies to 41. There are no obvious trends between the various measured global galaxy properties, particularly between mean surface brightness and galaxy mass.

Published
2023
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2. Impact of nationwide enhanced implementation of best practices in pancreatic cancer care (PACAP-1): a multicenter stepped-wedge cluster randomized controlled trial

Author

T. M. Mackay, F. J. Smits, A. E. J. Latenstein, A. Bogte, B. A. Bonsing, H. Bos, K. Bosscha, L. A. A. Brosens, L. Hol, O. R. C. Busch, G. J. Creemers, W. L. Curvers, M. den Dulk, S. van Dieren, L. M. J. W. van Driel, S. Festen, E. J. M. van Geenen, L. G. van der Geest, D. J. A. de Groot, J. W. B. de Groot, N. Haj Mohammad, B. C. M. Haberkorn, J. T. Haver, E. van der Harst, G. J. M. Hemmink, I. H. de Hingh, C. Hoge, M. Y. V. Homs, N. C. van Huijgevoort, M. A. J. M. Jacobs, E. D. Kerver, M. S. L. Liem, M. Los, H. Lubbinge, S. A. C. Luelmo, V. E. de Meijer, L. Mekenkamp, I. Q. Molenaar, M. G. H. van Oijen, G. A. Patijn, R. Quispel, L. B. van Rijssen, T. E. H. Römkens, H. C. van Santvoort, J. M. J. Schreinemakers, H. Schut, T. Seerden, M. W. J. Stommel, A. J. ten Tije, N. G. Venneman, R. C. Verdonk, J. Verheij, F. G. I. van Vilsteren, J. de Vos-Geelen, A. Vulink, C. Wientjes, F. Wit, F. J. Wessels, B. Zonderhuis, C. H. van Werkhoven, J. E. van Hooft, C. H. J. van Eijck, J. W. Wilmink, H. W. M. van Laarhoven, M. G. Besselink, and for the Dutch Pancreatic Cancer Group

Subjects
Pancreatic cancer, Survival, Quality of life, Stepped-wedge cluster randomized controlled trial, Implementation, Best practices, Medicine (General), R5-920
Abstract

Abstract Background Pancreatic cancer has a very poor prognosis. Best practices for the use of chemotherapy, enzyme replacement therapy, and biliary drainage have been identified but their implementation in daily clinical practice is often suboptimal. We hypothesized that a nationwide program to enhance implementation of these best practices in pancreatic cancer care would improve survival and quality of life. Methods/design PACAP-1 is a nationwide multicenter stepped-wedge cluster randomized controlled superiority trial. In a per-center stepwise and randomized manner, best practices in pancreatic cancer care regarding the use of (neo)adjuvant and palliative chemotherapy, pancreatic enzyme replacement therapy, and metal biliary stents are implemented in all 17 Dutch pancreatic centers and their regional referral networks during a 6-week initiation period. Per pancreatic center, one multidisciplinary team functions as reference for the other centers in the network. Key best practices were identified from the literature, 3 years of data from existing nationwide registries within the Dutch Pancreatic Cancer Project (PACAP), and national expert meetings. The best practices follow the Dutch guideline on pancreatic cancer and the current state of the literature, and can be executed within daily clinical practice. The implementation process includes monitoring, return visits, and provider feedback in combination with education and reminders. Patient outcomes and compliance are monitored within the PACAP registries. Primary outcome is 1-year overall survival (for all disease stages). Secondary outcomes include quality of life, 3- and 5-year overall survival, and guideline compliance. An improvement of 10% in 1-year overall survival is considered clinically relevant. A 25-month study duration was chosen, which provides 80% statistical power for a mortality reduction of 10.0% in the 17 pancreatic cancer centers, with a required sample size of 2142 patients, corresponding to a 6.6% mortality reduction and 4769 patients nationwide. Discussion The PACAP-1 trial is designed to evaluate whether a nationwide program for enhanced implementation of best practices in pancreatic cancer care can improve 1-year overall survival and quality of life. Trial registration ClinicalTrials.gov, NCT03513705 . Trial opened for accrual on 22th May 2018.

Published
2020
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4. FAPI PET versus FDG PET, CT or MRI for Staging Pancreatic-, Gastric- and Cholangiocarcinoma: Systematic Review and Head-to-Head Comparisons of Diagnostic Performances

Author

Sophie E. M. Veldhuijzen van Zanten, Kay J. Pieterman, Bas P. L. Wijnhoven, Ilanah J. Pruis, Bas Groot Koerkamp, Lydi M. J. W. van Driel, Frederik A. Verburg, and Maarten G. J. Thomeer

Subjects
FAPI PET, diagnostic performance, pancreatic carcinoma, gastric carcinoma, cholangiocarcinoma, Medicine (General), R5-920
Abstract

Introduction: There is a pressing demand for the development of cancer-specific diagnostic imaging tools, particularly for staging of pancreatic-, gastric- or cholangiocarcinoma, as current diagnostic imaging techniques, including CT, MRI and PET using FDG, are not fully adequate. The novel PET-tracer “FAPI” has the potential to visualize even small tumour deposits employing the tumour-specific expression of fibroblast-activating protein (FAP) in malignant cells. Methods: We performed a systematic review to select studies investigating the use of FAPI PET for staging pancreatic-, gastric- and cholangiocarcinoma (PROSPERO CRD42022329512). Patient-wise and lesion-wise comparisons were performed for primary tumour (T), lymph nodes (N), organ metastases (M) and peritoneal carcinomatosis (PC). Maximum standardized uptake values (SUVmax) and tumour-to-background ratios (TBR) were compared between PET using FAPI versus FDG (if reported). Results: Ten articles met the inclusion criteria. In all studies, FAPI PET showed superiority over FDG-PET/CT/MRI for the detection of T, N, M and PC, both in the patient-wise and in lesion-wise comparisons (when performed). Additionally, higher SUVmax and TBRmax values were reported for use of FAPI compared to FDG. Conclusions: The positive results of this review warrant prospective clinical studies to investigate the accuracy and clinical value of FAPI PET for diagnosing and staging patients with pancreatic-, gastric- and cholangiocarcinoma.

Published
2022
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6. Diagnostic yield and agreement on fine-needle specimens from solid pancreatic lesions: comparing the smear technique to liquid-based cytology

Author

Priscilla A. van Riet, Rutger Quispel, Djuna L. Cahen, Mieke C. Snijders-Kruisbergen, Petri van Loenen, Nicole S. Erler, Jan-Werner Poley, Lydi M. J. W. van Driel, Sanna A. Mulder, Bart J. Veldt, Ivonne Leeuwenburgh, Marie-Paule G. F. Anten, Pieter Honkoop, Annemieke Y. Thijssen, Lieke Hol, Mohammed Hadithi, Claire E. Fitzpatrick, Ingrid Schot, Jilling F. Bergmann, Abha Bhalla, Marco J. Bruno, and Katharina Biermann

Subjects
Diseases of the digestive system. Gastroenterology, RC799-869
Abstract

Background and study aims The traditional “smear technique” for processing and assessing endoscopic ultrasound-guided fine-needle aspiration (EUS-FNA) is sensitive to artifacts. Processing and evaluation of specimens collected in a liquid medium, liquid-based cytology (LBC) may be a solution. We compared the diagnostic value of EUS-FNA smears to LBC in pancreatic solid lesions in the absence of rapid on-site evaluation (ROSE). Patients and methods Consecutive patients who required EUS-FNA of a solid pancreatic lesion were included in seven hospitals in the Netherlands and followed for at least 12 months. Specimens from the first pass were split into two smears and a vial for LBC (using ThinPrep and/or Cell block). Smear and LBC were compared in terms of diagnostic accuracy for malignancy, sample quality, and diagnostic agreement between three cytopathologists. Results Diagnostic accuracy for malignancy was higher for LBC (82 % (58/71)) than for smear (66 % (47/71), P = 0.04), but did not differ when smears were compared to ThinPrep (71 % (30/42), P = 0.56) or Cell block (62 % (39/63), P = 0.61) individually. Artifacts were less often present in ThinPrep (57 % (24/42), P = 0.02) or Cell block samples (40 % (25/63), P

Published
2020
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8. Long-term yield of pancreatic cancer surveillance in high-risk individuals

Author

Kasper A, Overbeek, Iris J M, Levink, Brechtje D M, Koopmann, Femme, Harinck, Ingrid C A W, Konings, Margreet G E M, Ausems, Anja, Wagner, Paul, Fockens, Casper H, van Eijck, Bas, Groot Koerkamp, Olivier R C, Busch, Marc G, Besselink, Barbara A J, Bastiaansen, Lydi M J W, van Driel, Nicole S, Erler, Frank P, Vleggaar, Jan-Werner, Poley, Djuna L, Cahen, Jeanin E, van Hooft, Marco J, Bruno, M A, Kuenen, Surgery, Gastroenterology & Hepatology, Clinical Genetics, Epidemiology, Gastroenterology and Hepatology, CCA - Imaging and biomarkers, CCA - Cancer Treatment and Quality of Life, and AGEM - Amsterdam Gastroenterology Endocrinology Metabolism

Subjects
Oncology, medicine.medical_specialty, family cancer, pancreatic cancer, Endoscopic ultrasonography, Asymptomatic, SDG 3 - Good Health and Well-being, Pancreatic cancer, Internal medicine, medicine, Carcinoma, magnetic resonance imaging, Humans, Early Detection of Cancer, endoscopic ultrasonography, Genetic testing, medicine.diagnostic_test, business.industry, Incidence (epidemiology), Gastroenterology, Magnetic resonance imaging, Middle Aged, medicine.disease, digestive system diseases, Pancreatic Neoplasms, surveillance, Lifetime risk, medicine.symptom, business, Carcinoma, Pancreatic Ductal
Abstract

ObjectiveWe aimed to determine the long-term yield of pancreatic cancer surveillance in hereditary predisposed high-risk individuals.DesignFrom 2006 to 2019, we prospectively enrolled asymptomatic individuals with an estimated 10% or greater lifetime risk of pancreatic ductal adenocarcinoma (PDAC) after obligatory evaluation by a clinical geneticist and genetic testing, and subjected them to annual surveillance with both endoscopic ultrasonography (EUS) and MRI/cholangiopancreatography (MRI/MRCP) at each visit.Results366 individuals (201 mutation-negative familial pancreatic cancer (FPC) kindreds and 165 PDAC susceptibility gene mutation carriers; mean age 54 years, SD 9.9) were followed for 63 months on average (SD 43.2). Ten individuals developed PDAC, of which four presented with a symptomatic interval carcinoma and six underwent resection. The cumulative PDAC incidence was 9.3% in the mutation carriers and 0% in the FPC kindreds (pConclusionThe diagnostic yield of PDAC was substantial in established high-risk mutation carriers, but non-existent in the mutation-negative proven FPC kindreds. Nevertheless, timely identification of resectable lesions proved challenging despite the concurrent use of two imaging modalities, with EUS outperforming MRI/MRCP. Overall, surveillance by imaging yields suboptimal results with a clear need for more sensitive diagnostic markers, including biomarkers.

Published
2021

9. Comparison of Intraductal RFA Plus Stent versus Stent-Only Treatment for Unresectable Perihilar Cholangiocarcinoma—A Systematic Review and Meta-Analysis

Author

David M. de Jong, Jeska A. Fritzsche, Amber S. Audhoe, Suzanne S. L. Yi, Marco J. Bruno, Rogier P. Voermans, and Lydi M. J. W. van Driel

Subjects
Cancer Research, surgical procedures, operative, SDG 3 - Good Health and Well-being, Oncology, cardiovascular diseases, radiofrequency ablation, equipment and supplies, endoscopic stent, percutaneous stent, biliary drainage, unresectable perihilar cholangiocarcinoma
Abstract

Background: One of the cornerstones of palliative treatment for unresectable perihilar cholangiocarcinoma is biliary stent placement in order to restore biliary drainage. In this review, the potential added value of RFA with stent placement in comparison to stent placement alone in patients with unresectable perihilar cholangiocarcinoma is analyzed. Methods: We performed a comprehensive online search for relevant articles in November 2021 (PROSPERO ID: CRD42021288180). The primary endpoint was difference in overall survival. Secondary endpoints included overall survival, stent patency and complications. Only studies comparing survival after RFA + stent placement with stent placement alone were included in the meta-analysis. Non-comparative studies or comparative studies describing stent patency only were included in the systematic review. Results: A total of nine studies, including 217 patients with pCCA who underwent RFA + stent placement and 294 patients who underwent stent-only treatment, met the inclusion criteria for the primary endpoint analysis. Direct comparison between the two treatment groups showed a significantly longer overall survival for RFA + stent treatment, with a pooled HR of 0.65 [95% CI, 0.50–0.84, I2 = 38%]. When all eligible studies were included, RFA + stent treatment revealed an overall survival of 9.5 months [95% CI, 6.3–12.6], whereas survival for stent-only treatment was 7.0 months [95% CI, 5.7–8.2]. Due to the heterogeneity of the data, no pooled data analysis could be performed on stent patency or complications. Conclusions: RFA + stent placement displays promising potential to prolong survival. However, further research incorporating confounding factors like use of palliative chemotherapy is necessary in order to validate these findings.

Published
2022

10. A bivariate zero-inflated Poisson control chart: Comments and corrections on earlier results

Author

Edwin R. van den Heuvel, Zhuozhao Zhan, Stephan A. W. van Driel, Stochastic Operations Research, Mathematics and Computer Science, ICMS Core, and EAISI Foundational

Subjects
Statistics and Probability, 021103 operations research, 0211 other engineering and technologies, Statistics::Other Statistics, 02 engineering and technology, Bivariate analysis, Poisson distribution, Statistical process control, 01 natural sciences, Statistics::Computation, Copula (probability theory), 010104 statistics & probability, symbols.namesake, Copula, Statistics, Rare events, symbols, Zero-inflated model, Control chart, Zero inflated Poisson distribution, 0101 mathematics, Mathematics
Abstract

A bivariate zero-inflated Poisson control chart for rare events in an industrial process was presented in the paper of Fatahi et al. (2012). They used a specific copula to address the dependency between the bivariate counts. The copula that they provided did not satisfy the criteria for a copula when the correlation parameter is negative and they did not calculate the upper control limit for the sum of events correctly. We provide proper copula’s and upper control limits and also discuss their choice of parameter estimators. We illustrate our results with simulations.

Published
2020

11. Cherenkov Telescope Array : the World’s largest VHE gamma-ray observatory

Author

Roberta Zanin, H. Abdalla, H. Abe, S. Abe, A. Abusleme, F. Acero, A. Acharyya, V. Acin Portella, K. Ackley, R. Adam, C. Adams, S.S. Adhikari, I. Aguado Ruesga, I. Agudo, R. Aguilera, A. Aguirre Santaella, F. Aharonian, A. Alberdi, R. Alfaro, J. Alfaro, C. Alispach, R. Aloisio, R. Alves Batista, J.P. Amans, L. Amati, E. Amato, L. Ambrogi, G. Ambrosi, M. Ambrosio, R. Ammendola, J. Anderson, M. Anduze, E.O. Anguner, L.A. Antonelli, V. Antonuccio, P. Antoranz, R. Anutarawiramkul, J. Aragunde Gutierrez, C. Aramo, A. Araudo, M. Araya, A. Arbet Engels, C. Arcaro, V. Arendt, C. Armand, T. Armstrong, F. Arqueros, L. Arrabito, B. Arsioli, M. Artero, K. Asano, Y. Ascasibar, J. Aschersleben, M. Ashley, P. Attina, P. Aubert, C. B. Singh, D. Baack, A. Babic, M. Backes, V. Baena, S. Bajtlik, A. Baktash, C. Balazs, M. Balbo, O. Ballester, J. Ballet, B. Balmaverde, A. Bamba, R. Bandiera, A. Baquero Larriva, P. Barai, C. Barbier, V. Barbosa Martins, M. Barcelo, M. Barkov, M. Barnard, L. Baroncelli, U. Barres de Almeida, J.A. Barrio, D. Bastieri, P.I. Batista, I. Batkovic, C. Bauer, R. Bautista González, J. Baxter, U. Becciani, J. Becerra González, Y. Becherini, G. Beck, J. Becker Tjus, W. Bednarek, A. Belfiore, L. Bellizzi, R. Belmont, W. Benbow, D. Berge, E. Bernardini, M.I. Bernardos, K. Bernlöhr, A. Berti, M. Berton, B. Bertucci, V. Beshley, N. Bhatt, S. Bhattacharyya, W. Bhattacharyya, B. Y. Bi, G. Bicknell, N. Biederbeck, C. Bigongiari, A. Biland, R. Bird, E. Bissaldi, J. Biteau, M. Bitossi, O. Blanch, M. Blank, J. Blazek, J. Bobin, C. Boccato, F. Bocchino, C. Boehm, M. Bohacova, C. Boisson, J. Boix, J.P. Bolle, J. Bolmont, G. Bonanno, C. Bonavolontà, L. Bonneau Arbeletche, G. Bonnoli, P. Bordas, J. Borkowski, R. Bose, D. Bose, Z. Bosnjak, E. Bottacini, Markus Böttcher, M.T. Botticella, C. Boutonnet, F. Bouyjou, V. Bozhilov, E. Bozzo, L. Brahimi, C. Braiding, S. Brau Nogue, S. Breen, J. Bregeon, M. Breuhaus, A. Brill, W. Brisken, E. Brocato, A.M. Brown, K. Brügge, P. Brun, F. Brun, L. Brunetti, G. Brunetti, P. Bruno, A. Bruno, A. Bruzzese, N. Bucciantini, J. H. Buckley, R. Bühler, A. Bulgarelli, T. Bulik, M. Bünning, M. Bunse, M. Burton, A. Burtovoi, M. Buscemi, S. Buschjager, G. Busetto, J. Buss, K. Byrum, A. Caccianiga, F. Cadoux, A. Calanducci, C. Calderon, J. Calvo Tovar, R. A. Cameron, P. Campana, R. Canestrari, F. Cangemi, B. Cantlay, M. Capalbi, M. Capasso, M. Cappi, A. Caproni, R. Capuzzo Dolcetta, P. Caraveo, V. Cárdenas, L. Cardiel, M. Cardillo, C. Carlile, S. Caroff, R. Carosi, A. Carosi, E. Carquin, M. Carrere, J.M. Casandjian, S. Casanova, F. Cassol, F. Catalani, O. Catalano, D. Cauz, A. Ceccanti, C. Celestino Silva, K. Cerny, M. Cerruti, E. Chabanne, P. Chadwick, Y. Chai, P. Chambery, C. Champion, S. Chaty, A. Chen, K. Cheng, M. Chernyakova, G. Chiaro, A. Chiavassa, M. Chikawa, V.R. Chitnis, J. Chudoba, L. Chytka, S. Cikota, A. Circiello, P. Clark, M. Colak, E. Colombo, S. Colonges, A. Comastri, A. Compagnino, V. Conforti, E. Congiu, R. Coniglione, J. Conrad, F. Conte, J.L. Contreras, P. Coppi, R. Cornat, J. Coronado Blazquez, J. Cortina, A. Costa, H. Costantini, G. Cotter, B. Courty, S. Covino, S. Crestan, P. Cristofari, R. Crocker, J. Croston, K. Cubuk, O. Cuevas, X. Cui, G. Cusumano, S. Cutini, G. D'Amico, F. D'Ammando, P. D'Avanzo, P. Da Vela, M. Dadina, S. Dai, M. Dalchenko, M. Dall'Ora, M.K. Daniel, J. Dauguet, I. Davids, J. Davies, B. Dawson, A. De Angelis, A.E. de Araujo Carvalho, M. de Bony de Lavergne, G. De Cesare, F. de Frondat, I. de la Calle, E. de Gouveia Dal Pino, B. De Lotto, A. De Luca, D. De Martino, M. de Naurois, E. de Ona Wilhelmi, F. De Palma Persio, N. De Simone, V. de Souza Valle, E. Delagnes, G. Deleglise Reznicek, C. Delgado, A.G. Delgado Giler, J. Delgado Mengual Valle, Domenico Della Volpe, D. Depaoli, J. Devin, T. Di Girolamo, C. Di Giulio Pierro, L. Di Venere, C. Díaz, C. Dib, S. Diebold, S. Digel, A. Djannati Atai, J. Djuvsland, A. Dmytriiev, K. Docher, A. Domínguez, D. Dominis Prester, A. Donini, D. Dorner, M. Doro, Rita Cassia dos Anjos, J.L. Dournaux, T. Downes, G. Drake, H. Drass, D. Dravins, C. Duangchan, A. Duara, G. Dubus, L. Ducci, C. Duffy, D. Dumora, K. Dundas Mora, A. Durkalec, V.V. Dwarkadas, J. Ebr, C. Eckner, J. Eder, E. Edy, K. Egberts, S. Einecke, C. Eleftheriadis, D. Elsässer, G. Emery, D. Emmanoulopoulos, J.P. Ernenwein, M. Errando, P. Escarate, J. Escudero, C. Espinoza, S. Ettori, A. Eungwanichayapant, P. Evans, C. Evoli, M. Fairbairn, D. Falceta Goncalves, A. Falcone, V. Fallah Ramazanı, R. Falomo, K. Farakos, G. Fasola, A. Fattorini, Y. Favre, R. Fedora, E. Fedorova, K. Feijen, Q. Feng, G. Ferrand, G. Ferrara, O. Ferreira, M. Fesquet, E. Fiandrini, A. Fiasson, M. Filipovic, D. Fink, J.P. Finley, V. Fioretti, D.F.G. Fiorillo, M. Fiorini, S. Flis, H. Flores, L. Foffano, C. Fohr, M.V. Fonseca, L. Font, G. Fontaine, O. Fornieri, P. Fortin, L. Fortson, N. Fouque, B. Fraga, A. Franceschini, F.J. Franco, L. Freixas Coromina, L. Fresnillo, D. Fugazza, Y. Fujita, S. Fukami, Y. Fukazawa, D. Fulla, S. Funk, A. Furniss, S. Gabici, D. Gaggero, G. Galanti, P. Galdemard, Y. A. Gallant, D. Galloway, S. Gallozzi, V. Gammaldi, R. Garcia, L. E. García-Muñoz, E. Garcia Lopez, F. Gargano, C. Gargano, S. Garozzo, D. Gascon, T. Gasparetto, D. Gasparrini, H. Gasparyan, M. Gaug, N. Geffroy, A. Gent, S. Germani, A. Ghalumyan, A. Ghedina, G. Ghirlanda, F. Gianotti, S. Giarrusso, M. Giarrusso, G. Giavitto, B. Giebels, N. Giglietto, V. Gika, F. Gillardo, R. Gimenes, F. Giordano, E. Giro, M. Giroletti, Andrea Giuliani, M. Gjaja, J.F. Glicenstein, P. Gliwny, H. Goksu, P. Goldoni, J.L. Gomez, M.M. Gonzalez, Juan Manuel Gonzalez, K.S. Gothe, D. Gotz Coelho, T. Grabarczyk, R. Graciani, P. Grandi, G. Grasseau, D. Grasso, D. Green, J. Green, T. Greenshaw, P. Grespan, A. Grillo, M.H. Grondin, J. Grube, V. Guarino, B. Guest, O. Gueta, M. Günduz, S. Gunji, G. Gyuk, J. Hackfeld, D. Hadasch, L. Hagge, A. Hahn, J.E. Hajlaoui, A. Halim, P. Hamal, W. Hanlon, Y. Harada, M.J. Hardcastle, M. Harvey Collado, T. Haubold, A. Haupt, M. Havelka, K. Hayashi, M. Hayashida, H. He, L. Heckmann, M. Heller, F. Henault, Gilles Henri, G. Hermann, S. Hernández Cadena, J. Herrera Llorente, O. Hervet, J. Hinton, A. Hiramatsu, K. Hirotani, B. Hnatyk, R. Hnatyk, J.K. Hoang, D. H.H. Hoffmann, C. Hoischen, J. Holder, M. Holler, B. Hona, D. Horan, Dieter Horns, P. Horvath, J. Houles, M. Hrabovsky, D. Hrupec, Y. Huang, J.‑M. Huet, G. Hughes, G. Hull, T.B. Humensky, M. Hütten, M. Iarlori, J.M. Illa, R. Imazawa, T. Inada, F. Incardona, A. Ingallinera, S. Inoue, T. Inoue, Y. Inoue, F. Iocco, K. Ioka, M. Ionica, S. Iovenitti, A. Iriarte, K. Ishio, W. Ishizaki, Y. Iwamura, J. Jacquemier, M. Jacquemont, M. Jamrozy, P. Janecek, F. Jankowsky, A. JardinBlicq, C. Jarnot, P. Jean Martínez, L. Jocou, N. Jordana, M. Josselin, I. JungRichardt, F.J.P.A. Junqueira, C. Juramy Gilles, P. Kaaret, L.H.S. Kadowaki, M. Kagaya, R. Kankanyan, D. Kantzas, V. Karas, A. Karastergiou, S. Karkar, J. Kasperek, H. Katagiri, J. Kataoka, K. Katarzynski, S. Katsuda, N. Kawanaka, D. Kazanas, D. Kerszberg, B. Khélifi, M.C. Kherlakian, T.P. Kian, D.B. Kieda, T. Kihm, S. Kim, S. Kisaka, R. Kissmann, R. Kleijwegt, G. Kluge, W. Kluźniak, J. Knapp, A. Kobakhidze, Y. Kobayashi, B. Koch, J. Kocot, K. Kohri, N. Komin, A. Kong, K. Kosack, F. Krack, M. Krause, F. Krennrich, H. Kubo, V. N. Kudryavtsev, S. Kunwar, J. Kushida, P. Kushwaha, Barbera Parola, G. La Rosa, R. Lahmann, A. Lamastra, M. Landoni, D. Landriu, R.G. Lang, J. Lapington, P. Laporte, P. Lason, J. Lasuik, J. Lazendic Galloway, T. Le Flour, P. Le Sidaner, S. Leach, S.H. Lee, W.H. Lee, S. Lee Oliveira, A. Lemiere, M. Lemoine Goumard, J.P. Lenain, F. Leone, V. Leray, G. Leto, F. Leuschner, R. Lindemann, E. Lindfors, L. Linhoff, I. Liodakis, A. Lipniacka, M. Lobo, Thomas Lohse, S. Lombardi, A. Lopez, M. Lopez, R. Lopez Coto, F. Louis, M. Louys, F. Lucarelli, H. Ludwig Boudi, P.L. Luque Escamilla, M.C. Maccarone, E. Mach, A.J. Maciejewski, J. Mackey, P. Maeght, C. Maggio, G. Maier, P. Majumdar, M. Makariev, M. Mallamaci, R. Malta Nunes de Almeida, D. Malyshev, D. Mandat, G. Maneva, M. Manganaro, P. Manigot, K. Mannheim, N. Maragos, D. Marano, M. Marconi, A. Marcowith, M. Marculewicz, B. Marcun, J. Marin, N. Marinello, P. Marinos, S. Markoff, P. Marquez, G. Marsella, J. M. Martin, P. G. Martin, M. Martinez, G. Martinez, O. Martinez, H. Martinez Huerta, C. Marty, R. Marx, N. Masetti, P. Massimino, H. Matsumoto, N. Matthews, G. Maurin, W. Max Moerbeck, N. Maxted, M.N. Mazziotta, S.M. Mazzola, J.D. Mbarubucyeye, L. Mc Comb, I. McHardy, S. McKeague, S. McMuldroch, E. Medina, D. Medina Miranda, A. Melandri, C. Melioli, D. Melkumyan, S. Menchiari, S. Mereghetti, G. Merino Arevalo, E. Mestre, J.L. Meunier, T. Meures, S. Micanovic, M. Miceli, M. Michailidis, J. Michalowski, T. Miener, I. Mievre, J. D. Miller, T. Mineo, M. Minev, J.M. Miranda, A. Mitchell, T. Mizuno, B. A. Mode, R. Moderski, L. Mohrmann, E. Molinari, T. Montaruli, I. Monteiro, C. Moore, A. Moralejo, D. Morcuende Parrilla, E. Moretti, K. Mori, P. Moriarty, K. Morik, P. Morris, A. Morselli, K. Mosshammer, R. Mukherjee, J. Muller, C. Mundell, J. Mundet, T. Murach, A. Muraczewski, H. Muraishi, I. Musella, A. Musumarra, A. Nagai, S. Nagataki, T. Naito, T. Nakamori, K. Nakashima, K. Nakayama, N. Nakhjiri, G. Naletto, D. Naumann, L. Nava, M.A. Nawaz, H. Ndiyavala, D. Neise, L. Nellen, R. Nemmen, N. Neyroud, K. Ngernphat, T. Nguyen Trung, L. Nicastro, L. Nickel, J. Niemiec, D. Nieto, C. Nigro, M. Nikołajuk, D. Ninci, K. Noda, Y. Nogami, S. Nolan, R. P. Norris, D. Nosek, M. Nöthe, V. Novotny, S. Nozaki, F. Nunio, P. O'Brien, K. Obara, Y. Ohira, M. Ohishi, S. Ohm, T. Oka, N. Okazaki, A. Okumura, C. Oliver, G. Olivera, B. Olmi, M. Orienti, R. Orito, M. Orlandini, E. Orlando, J.P. Osborne, M. Ostrowski, N. Otte, E. Ovcharov, E. Owen, I. Oya, A. Ozieblo, M. Padovani, A. Pagliaro, A. Paizis, M. Palatiello, M. Palatka, E. Palazzi, J.‑L. Panazol, D. Paneque, S. Panny, Francesca Romana Pantaleo, M. Panter, M. Paolillo, A. Papitto, A. Paravac, J.M. Paredes, G. Pareschi, N. Parmiggiani, R.D. Parsons, P. Paśko, S. R. Patel, B. Patricelli, L. Pavletic, S. Pavy, A. Peer, M. Pecimotika, M.G. Pellegriti, P. Peñil Del Campo, A. Pepato, S. Perard, C. Perennes, M. Peresano, A. Perez Aguilera, J. Perez Romero, M.A. Perez Torres, M. Persic, P. O. Petrucci, O. Petruk, B. Peyaud, K. Pfrang, E. Pian, P. Piatteli, E. Pietropaolo, R. Pillera, D. Pimentel, F. Pintore, C. Pio Garcia, G. Pirola, F. Piron, S. Pita, M. Pohl, V. Poireau, A. Pollo, M. Polo, C. Pongkitivanichkul, J. Porthault, J. Powell, D. Pozo, R.R. Prado, E. Prandini, J. Prast, K. Pressard, G. Principe, N. Produit, D. Prokhorov, H. Prokoph, H. Przybilski, E. Pueschel, G. Pühlhofer, I. Puljak, M.L. Pumo, M. Punch, F. Queiroz, J. Quinn, A. Quirrenbach, P.J. Rajda, R. Rando, S. Razzaque, S. Recchia, P. Reichherzer, O. Reimer, A. Reisenegger, Q. Remy, M. Renaud, T. Reposeur, B. Reville, J.M. Reymond, J. Reynolds, D. Ribeiro, M. Ribo, G. Richards, J. Rico, F. Rieger, L. Riitano, M. Riquelme, D. Riquelme, S. Rivoire, V. Rizi, E. Roache, M. Roche, J. Rodriguez, G. Rodriguez Fernandez, J.C. Rodriguez Ramirez, J.J. Rodriguez Vazquez, G. Rojas, P. Romano, G. Romeo Lobato, C. Romoli, M. Roncadelli, J. Rosado, A. Rosales de Leon, G. Rowell, A. Rugliancich, J.E. Ruiz del Mazo, C. Rulten, C. Russell, F. Russo Hatlen, S. Safi Harb, L. Saha, V. Sahakian, S. Sailer, T. Saito, N. Sakaki, S. Sakurai, G. Salina, H. Salzmann, D. Sanchez, H. Sandaker, A. Sandoval, P. Sangiorgi, M. Sanguillon, H. Sano, M. Santander, A. Santangelo, R. Santos Lima, A. Sanuy, L. Sapozhnikov, T. Saric, S. Sarkar, H. Sasaki, N. Sasaki, Y. Sato, F.G. Saturni, M. Sawada, J. Schaefer, A. Scherer, J. Scherpenberg, P. Schipani, B. Schleicher, J. Schmoll, M. Schneider, H. Schoorlemmer, P. Schovanek, F. Schussler, B. Schwab, U. Schwanke, J. Schwarz, E. Sciacca, S. Scuderi, M. Seglar Arroyo, I. Seitenzahl, D. Semikoz, O. Sergijenko, J.E. Serna Franco, Karol Seweryn, V. Sguera, A. Shalchi, R.Y. Shang, P. Sharma, L. Sidoli, J. Sieiro, H. Siejkowski, A. Sillanpaa, B.B. Singh, K.K. Singh, A. Sinha, C. Siqueira, J. Sitarek, P. Sizun, V. Sliusar, D. Sobczynska, R.W. Sobrinho, H. Sol, G. Sottile, H. Spackman, S. Spencer, G. Spengler, D. Spiga, W. Springer, A. Stamerra, S. Stanic, R. Starling, Ł. Stawarz, Stanislav Stefanik, C. Stegmann, A. Steiner, S. Steinmassl, C. Stella, R. Sternberger, M. Sterzel, C. Stevens, B. Stevenson, T. Stolarczyk, G. Stratta, U. Straumann, J. Striskovic, M. Strzys, R. Stuik, M. Suchenek, Y. Sunada, Tiina Suomijarvi, T. Suric, H. Suzuki, P. Swierk, T. Szepieniec, K. Tachihara, G. Tagliaferri, H. Tajima, N. Tajima, D. Tak, H. Takahashi, M. Takahashi, J. Takata, R. Takeishi, T. Tam, M. Tanaka, T. Tanaka, S. Tanaka, M. Tavani, F. Tavecchio, T. Tavernier, A. Russ Taylor, L.A. Tejedor, P. Temnikov, K. Terauchi, J.C. Terrazas, R. Terrier, T. Terzic, M. Teshima, D. Thibaut, F. Thocquenne, W. Tian, L. Tibaldo, A. Tiengo, M. Tluczykont, C.J. Todero Peixoto, K. Toma, L. Tomankova, J. Tomastik, M. Tornikoski, D.F. Torres, E. Torresi, G. Tosti, L. Tosti, N. Tothill, F. Toussenel, G. Tovmassian, C. Trichard, M. Trifoglio, A. Trois, S. Truzzi, A. Tsiahina, B. Turk, A. Tutone, Y. Uchiyama, P. Utayarat, L. Vaclavek, M. Vacula, V. Vagelli, F. Vagnetti, J.A. Valdivia, M. Valentino, A. Valio, B. Vallage, P. Vallania Quispe, A.M. van den Berg, W. van Driel, C. van Eldik, C. van Rensburg, Brian van Soelen, J. Vandenbroucke, G. Vasileiadis, V. Vassiliev, M. Vazquez Acosta, M. Vecchi, A. Vega, J. Veh, P. Veitch, C. Venter, S. Ventura, S. Vercellone, V. Verguilov, G. Verna, S. Vernetto, V. Verzi, G.P. Vettolani, C. Veyssiere, I. Viale, A. Viana, N. Viaux, J. Vignatti, C.F. Vigorito, J. Villanueva, V. Vitale, V. Vittorini, V. Vodeb, N. Vogel, V. Voisin, S. Vorobiov, M. Vrastil, T. Vuillaume, S.J. Wagner, P. Wagner, K. Wakazono, S.P. Wakely, M. Ward, D. Warren, J. Watson, M. Wechakama, P. Wegner, A. Weinstein, C. Weniger, F. Werner, H. Wetteskind, M. L. White, A. Wierzcholska, S. Wiesand, R. Wijers, M. Wilkinson, M. Will, J. Williams, T. J. Williamson, A. Wolter, Y.W. Wong, M. Wood, T. Yamamoto, H. Yamamoto, Y. Yamane, R. Yamazaki, S. Yanagita, L. Yang, S. Yoo, T. Yoshida, T. Yoshikoshi, P. Yu, A. Yusafzai, Michael Zacharias, B. Zaldivar, L. Zampieri, R. Zanin, R. Zanmar Sanchez, D. Zaric, M. Zavrtanik, D. Zavrtanik, Andrzej Zdziarski, A. Zech, H. Zechlin, A. Zenin, A. Zerwekh, K. Ziętara, A. Zink, J. Ziolkowski, M. Zivec, A. Zmija, Współautorami artykułu są członkowie CTA Observatory, CTA Consortium i LST Collaboration w liczbie 1139, Astronomy, Research unit Nuclear & Hadron Physics, and Research unit Astroparticle Physics

Subjects
Physics, Observatory, Gamma ray, Astronomy
Abstract

Very-high Energy (VHE) gamma-ray astroparticle physics is a relatively young field, and observations over the past decade have surprisingly revealed almost two hundred VHE emitters which appear to act as cosmic particle accelerators. These sources are an important component of the Universe, influencing the evolution of stars and galaxies. At the same time, they also act as a probe of physics in the most extreme environments known - such as in supernova explosions, and around or after the merging of black holes and neutron stars. However, the existing experiments have provided exciting glimpses, but often falling short of supplying the full answer. A deeper understanding of the TeV sky requires a significant improvement in sensitivity at TeV energies, a wider energy coverage from tens of GeV to hundreds of TeV and a much better angular and energy resolution with respect to the currently running facilities. The next generation gamma-ray observatory, the Cherenkov Telescope Array Observatory (CTAO), is the answer to this need. In this talk I will present this upcoming observatory from its design to the construction, and its potential science exploitation. CTAO will allow the entire astronomical community to explore a new discovery space that will likely lead to paradigm-changing breakthroughs. In particular, CTA has an unprecedented sensitivity to short (sub-minute) timescale phenomena, placing it as a key instrument in the future of multi-messenger and multi-wavelength time domain astronomy. I will conclude the talk presenting the first scientific results obtained by the LST-1, the prototype of one CTAO telescope type - the Large-Sized Telescope, that is currently under commission., PoS: Proceedings of Science, 395, ISSN:1824-8039, Proceedings of 37th International Cosmic Ray Conference (ICRC2021)

Published
2022

12. Self-expandable duodenal metal stent placement for the palliation of gastric outlet obstruction over the past 20 years

Author

Agnes N. Reijm, Pauline A. Zellenrath, Ruben D. van der Bogt, Lydi M. J. W. van Driel, Peter D. Siersema, Marco J. Bruno, Manon C. W. Spaander, and Gastroenterology & Hepatology

Subjects
Male, Gastric Outlet Obstruction, Palliative Care, Gastroenterology, Self Expandable Metallic Stents, Constriction, Pathologic, Middle Aged, Tumours of the digestive tract Radboud Institute for Health Sciences [Radboudumc 14], Treatment Outcome, SDG 3 - Good Health and Well-being, Stomach Neoplasms, Humans, Female, Retrospective Studies, Aged
Abstract

Introduction Duodenal stent placement is a palliative option for management of malignant gastric outlet obstruction (GOO). In the last 20 years, management of gastrointestinal cancers has considerably changed. It is unknown if these changes have affected clinical outcome of duodenal stent placement. Methods Retrospective cohort study conducted in a tertiary referral center. Patients who underwent duodenal stent placement for GOO-symptoms due to a malignant stricture were included. Primary outcome was GOO-symptom free survival. Secondary outcomes included stent-related adverse event rates. Potential explanatory parameters such as period of stent placement (1998–2009 vs 2010–2019), prior treatments, peritoneal deposits, and stricture length were evaluated using multivariable Cox regression analysis. Results A total of 147 patients (62 % male; median age 64 years) were included. After a median of 28 days after stent placement, 82 patients (57 %) had recurrent GOO-symptoms. GOO-symptom free survival was significantly lower in 2010–2019 (P Conclusions Clinical outcome of duodenal stent placement did not improve over time. The decreased GOO-symptom free survival and increased adverse event rate in more recent years are probably related to the chemo- and/or radiotherapy treatment provided prior to duodenal stent placement.

Published
2022

13. Cumulative sum learning curves guiding multicenter multidisciplinary quality improvement of EUS-guided tissue acquisition of solid pancreatic lesions

Author

Hannah M, Schutz, Rutger, Quispel, Bart J, Veldt, Frank M M, Smedts, Marie-Paule G F, Anten, Klaas J, Hoogduin, Pieter, Honkoop, Francien H, van Nederveen, Lieke, Hol, Mike, Kliffen, Claire E, Fitzpatrick, Nicole S, Erler, Marco J, Bruno, Lydi M J W, van Driel, Epidemiology, and Gastroenterology & Hepatology

Subjects
Pharmacology (medical)
Abstract

Background and study aims In this study, we evaluated the performance of community hospitals involved in the Dutch quality in endosonography team regarding yield of endoscopic ultrasound (EUS)-guided tissue acquisition (TA) of solid pancreatic lesions using cumulative sum (CUSUM) learning curves. The aims were to assess trends in quality over time and explore potential benefits of CUSUM as a feedback-tool. Patients and methods All consecutive EUS-guided TA procedures for solid pancreatic lesions were registered in five community hospitals between 2015 and 2018. CUSUM learning curves were plotted for overall performance and for performance per center. The American Society of Gastrointestinal Endoscopy-defined key performance indicators, rate of adequate sample (RAS), and diagnostic yield of malignancy (DYM) were used for this purpose. Feedback regarding performance was provided on multiple occasions at regional interest group meetings during the study period. Results A total of 431 EUS-guided TA procedures in 403 patients were included in this study. The overall and per center CUSUM curves for RAS improved over time. CUSUM curves for DYM revealed gradual improvement, reaching the predefined performance target (70 %) overall, and in three of five contributing centers in 2018. Analysis of a sudden downslope development in the CUSUM curve of DYM in one center revealed temporary absence of a senior cytopathologist to have had a temporary negative impact on performance. Conclusions CUSUM-derived learning curves allow for assessment of best practices by comparison among peers in a multidisciplinary multicenter quality improvement initiative and proved to be a valuable and easy-to-interpret means to evaluate EUS performance over time.

Published
2021

14. hiss, a new tool for H i stacking: application to NIBLES spectra

Author

Robert F. Minchin, J. Healy, Matthew D. Lehnert, W. van Driel, Edward C. Elson, Z. Butcher, Stephen E. Schneider, S. L. Blyth, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Unité Scientifique de la Station de Nançay (USN), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université d'Orléans (UO), and Kapteyn Astronomical Institute

Subjects
statistical -galaxies, Hiss, Stellar mass, Stacking, FOS: Physical sciences, ARECIBO SDSS SURVEY, Astrophysics, I, 01 natural sciences, Spectral line, STAR-FORMATION, FRACTION, methods, Methods statistical, galaxies, 0103 physical sciences, 010303 astronomy & astrophysics, radio lines: galaxies, Physics, methods: statistical, ENVIRONMENT, 010308 nuclear & particles physics, GAS CONTENT, Astronomy and Astrophysics, HYDROGEN, methods: data analysis, galaxies: general, Astrophysics - Astrophysics of Galaxies, EVOLUTION, Galaxy, evolution -galaxies, general -radio lines, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Data analysis, DIGITAL SKY SURVEY, data analysis -methods, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Order of magnitude
Abstract

H I stacking has proven to be a highly effective tool to statistically analyse average H I properties for samples of galaxies which may or may not be directly detected. With the plethora of H I data expected from the various upcoming H I surveys with the SKA Precursor and Pathfinder telescopes, it will be helpful to standardize the way in which stacking analyses are conducted. In this work we present a new PYTHON-based package, HISS, designed to stack H I (emission and absorption) spectra in a consistent and reliable manner. As an example, we use HISS to study the H I content in various galaxy sub-samples from the NIBLES survey of SDSS galaxies which were selected to represent their entire range in total stellar mass without a prior colour selection. This allowed us to compare the galaxy colour to average H I content in both detected and non-detected galaxies. Our sample, with a stellar mass range of 10^8 \lt {{ M}}_\star (M_\odot) \lt 10^{12}, has enabled us to probe the H I-to-stellar mass gas fraction relationship more than half an order of magnitude lower than in previous stacking studies., Comment: 40 pages (of which 23 pages are appendices), 28 figures, 5 tables, published in MNRAS

Published
2019

15. Correction: The inactivation mechanism of chemical disinfection against SARS-CoV-2: from MD and DFT perspectives

Author

Chunjian Tan, W. Van Driel, G.Q. Zhang, Quan Zhou, Huaiyu Ye, and Chenshan Gao

Subjects
2019-20 coronavirus outbreak, Coronavirus disease 2019 (COVID-19), biology, Chemistry, Mechanism (biology), Severe acute respiratory syndrome coronavirus 2 (SARS-CoV-2), General Chemical Engineering, biology.protein, Chromatin structure remodeling (RSC) complex, General Chemistry, Virology, Chemical disinfection
Abstract

The authors regret that one of the affiliations (affiliation f) was incorrectly omitted in the original manuscript. The corrected list of affiliations is as shown below. The Royal Society of Chemistry apologises for these errors and any consequent inconvenience to authors and readers.

Published
2021
Full Text
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16. Challenges in Diagnosing Cholangiocarcinoma: Pulling Together Biochemical, Radiological, and Cytopathological Data

Author

S. Franssen, L. M. J. W. van Driel, B. Groot Koerkamp, and D. M. de Jong

Subjects
medicine.medical_specialty, medicine.diagnostic_test, business.industry, General surgery, Radiological weapon, medicine, Locally advanced, Adenocarcinoma, Physical examination, Medical history, Disease, medicine.disease, business
Abstract

The aim of the diagnostic work-up of cholangiocarcinoma (CCA) is diagnosis and staging of the disease as (borderline) resectable, locally advanced (i.e., unresectable), or metastatic. The focus of this chapter is on the various challenges often encountered in this diagnostic work-up. For instance, one major challenge is that CCA involves three disease entities that differ in genomic alterations, signs, and symptoms: intrahepatic (iCCA), perihilar (pCCA), and distal cholangiocarcinoma (dCCA). A second challenge is that it is frequently difficult to obtain adequate tissue for a definitive diagnosis. A third challenge is that several nonmalignant diseases can masquerade as CCA. These and other challenges are illustrated herein with a series of case presentations which also help highlight the importance of a multidisciplinary effort of gastroenterologists, surgeons, medical oncologists, radiologists, and pathologists. In some cases, despite a meticulous patient history, physical examination, and evaluation of imaging and laboratory tests by multidisciplinary experts, a diagnosis cannot be established with absolute certainty, and treatment may sometimes be started based on CCA being the most likely diagnosis.

Published
2021

17. Impact of nationwide enhanced implementation of best practices in pancreatic cancer care (PACAP-1):A multicenter stepped-wedge cluster randomized controlled trial

Author

B.M. Zonderhuis, Tom C.J. Seerden, N. C. M. van Huijgevoort, E. J. M. van Geenen, Leonie J. M. Mekenkamp, Koop Bosscha, C. Wientjes, R. C. Verdonk, Gijs A. Patijn, Rutger Quispel, L.G.M. van der Geest, Lodewijk A.A. Brosens, Frank J. Wessels, M. G. H. van Oijen, O.R.C. Busch, A. Bogte, Johanna W. Wilmink, Emile D. Kerver, Lieke Hol, Tara M. Mackay, J. Verheij, H. Lubbinge, Marjolein Y.V. Homs, I. Q. Molenaar, A.J. ten Tije, B. C. M. Haberkorn, Jennifer M.J. Schreinemakers, V E de Meijer, C.H. van Werkhoven, H.C. van Santvoort, Saskia A C Luelmo, Wouter L. Curvers, C.H.J. van Eijck, F.J. Smits, J. E. van Hooft, F. G. I. van Vilsteren, L. M. J. W. van Driel, F. Wit, Derk Jan A. de Groot, J. T. Haver, Bert A. Bonsing, H. Schut, I.H.J.T. de Hingh, J.W.B. de Groot, N. Haj Mohammad, H.W.M. van Laarhoven, H. Bos, Niels G. Venneman, M. den Dulk, L.B. van Rijssen, Martijn W J Stommel, Sebastiaan Festen, Tessa E H Römkens, Chantal V Hoge, Annelie Vulink, J. de Vos-Geelen, Gjm Hemmink, Marc Jacobs, G.J.M. Creemers, Anouk E J Latenstein, S. van Dieren, Marc G. Besselink, Mike Liem, E. van der Harst, Maartje Los, Surgery, AGEM - Digestive immunity, AGEM - Endocrinology, metabolism and nutrition, AGEM - Re-generation and cancer of the digestive system, CCA - Cancer Treatment and Quality of Life, APH - Methodology, Oncology, APH - Quality of Care, Ear, Nose and Throat, Graduate School, Pathology, Gastroenterology and Hepatology, CCA -Cancer Center Amsterdam, Gastroenterology and hepatology, CCA - Cancer Treatment and quality of life, Amsterdam Gastroenterology Endocrinology Metabolism, Groningen Institute for Organ Transplantation (GIOT), Center for Liver, Digestive and Metabolic Diseases (CLDM), Guided Treatment in Optimal Selected Cancer Patients (GUTS), Gastroenterology & Hepatology, Medical Oncology, MUMC+: MA Heelkunde (9), RS: NUTRIM - R2 - Liver and digestive health, Interne Geneeskunde, MUMC+: MA Maag Darm Lever (9), RS: GROW - R3 - Innovative Cancer Diagnostics & Therapy, and MUMC+: MA Medische Oncologie (9)

Subjects
Male, Survival, Medicine (miscellaneous), GUIDELINES, law.invention, Tumours of the digestive tract Radboud Institute for Health Sciences [Radboudumc 14], Study Protocol, 0302 clinical medicine, Superiority Trial, Randomized controlled trial, DESIGN, law, Tumours of the digestive tract Radboud Institute for Molecular Life Sciences [Radboudumc 14], Cluster Analysis, Multicenter Studies as Topic, Pharmacology (medical), 030212 general & internal medicine, Child, Netherlands, Randomized Controlled Trials as Topic, Aged, 80 and over, lcsh:R5-920, Pancreatic enzyme replacement therapy, STATEMENT, Palliative Care, Middle Aged, Neoadjuvant Therapy, Biliary Tract Surgical Procedures, Treatment Outcome, 030220 oncology & carcinogenesis, Child, Preschool, Drainage, Female, Stents, lcsh:Medicine (General), Carcinoma, Pancreatic Ductal, Adult, Quality of life, medicine.medical_specialty, Best practices, Registry, RESECTION, Referral, Adolescent, Best practice, Other Research Radboud Institute for Molecular Life Sciences [Radboudumc 0], Biliary drainage, Disease cluster, Pancreaticoduodenectomy, 03 medical and health sciences, Young Adult, Quality of life (healthcare), SDG 3 - Good Health and Well-being, Pancreatic cancer, medicine, Journal Article, Humans, Chemotherapy, Enzyme Replacement Therapy, Stepped-wedge cluster randomized controlled trial, Aged, business.industry, Health Plan Implementation, Infant, Newborn, Infant, Guideline, medicine.disease, Pancreatic Neoplasms, SAMPLE-SIZE, Implementation, Emergency medicine, Patient Compliance, business
Abstract

Background Pancreatic cancer has a very poor prognosis. Best practices for the use of chemotherapy, enzyme replacement therapy, and biliary drainage have been identified but their implementation in daily clinical practice is often suboptimal. We hypothesized that a nationwide program to enhance implementation of these best practices in pancreatic cancer care would improve survival and quality of life. Methods/design PACAP-1 is a nationwide multicenter stepped-wedge cluster randomized controlled superiority trial. In a per-center stepwise and randomized manner, best practices in pancreatic cancer care regarding the use of (neo)adjuvant and palliative chemotherapy, pancreatic enzyme replacement therapy, and metal biliary stents are implemented in all 17 Dutch pancreatic centers and their regional referral networks during a 6-week initiation period. Per pancreatic center, one multidisciplinary team functions as reference for the other centers in the network. Key best practices were identified from the literature, 3 years of data from existing nationwide registries within the Dutch Pancreatic Cancer Project (PACAP), and national expert meetings. The best practices follow the Dutch guideline on pancreatic cancer and the current state of the literature, and can be executed within daily clinical practice. The implementation process includes monitoring, return visits, and provider feedback in combination with education and reminders. Patient outcomes and compliance are monitored within the PACAP registries. Primary outcome is 1-year overall survival (for all disease stages). Secondary outcomes include quality of life, 3- and 5-year overall survival, and guideline compliance. An improvement of 10% in 1-year overall survival is considered clinically relevant. A 25-month study duration was chosen, which provides 80% statistical power for a mortality reduction of 10.0% in the 17 pancreatic cancer centers, with a required sample size of 2142 patients, corresponding to a 6.6% mortality reduction and 4769 patients nationwide. Discussion The PACAP-1 trial is designed to evaluate whether a nationwide program for enhanced implementation of best practices in pancreatic cancer care can improve 1-year overall survival and quality of life. Trial registration ClinicalTrials.gov, NCT03513705. Trial opened for accrual on 22th May 2018.

Published
2020

18. Additional file 1 of Impact of nationwide enhanced implementation of best practices in pancreatic cancer care (PACAP-1): a multicenter stepped-wedge cluster randomized controlled trial

Author

Mackay, T. M., F. J. Smits, A. E. J. Latenstein, A. Bogte, B. A. Bonsing, H. Bos, K. Bosscha, L. A. A. Brosens, L. Hol, O. R. C. Busch, G. J. Creemers, W. L. Curvers, M. Den Dulk, S. Van Dieren, L. M. J. W. Van Driel, S. Festen, E. J. M. Van Geenen, L. G. Van Der Geest, D. J. A. De Groot, J. W. B. De Groot, N. Haj Mohammad, B. C. M. Haberkorn, J. T. Haver, E. Van Der Harst, G. J. M. Hemmink, I. H. De Hingh, C. Hoge, M. Y. V. Homs, N. C. Van Huijgevoort, M. A. J. M. Jacobs, E. D. Kerver, M. S. L. Liem, M. Los, H. Lubbinge, S. A. C. Luelmo, V. E. De Meijer, L. Mekenkamp, I. Q. Molenaar, M. G. H. Van Oijen, G. A. Patijn, R. Quispel, L. B. Van Rijssen, T. E. H. Römkens, H. C. Van Santvoort, J. M. J. Schreinemakers, H. Schut, T. Seerden, M. W. J. Stommel, A. J. Ten Tije, N. G. Venneman, R. C. Verdonk, J. Verheij, F. G. I. Van Vilsteren, J. De Vos-Geelen, A. Vulink, C. Wientjes, F. Wit, F. J. Wessels, B. Zonderhuis, C. H. Van Werkhoven, J. E. Van Hooft, C. H. J. Van Eijck, J. W. Wilmink, H. W. M. Van Laarhoven, and M. G. Besselink

Abstract

Additional file 1. SPIRIT 2013 Checklist for the PACAP-1 trial.

Published
2020
Full Text
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19. Psychiatric characteristics of older persons with medically unexplained symptoms: A comparison with older patients suffering from medically explained symptoms

Author

Peter Lucassen, T J W van Driel, T.C. Olde Hartman, Denise Hanssen, R. C. Oude Voshaar, C.E.M. Benraad, Peter H. Hilderink, Paul Naarding, Interdisciplinary Centre Psychopathology and Emotion regulation (ICPE), and Clinical Cognitive Neuropsychiatry Research Program (CCNP)

Subjects
Adult, Male, medicine.medical_specialty, somatization, Comorbidity, Healthcare improvement science Radboud Institute for Health Sciences [Radboudumc 18], All institutes and research themes of the Radboud University Medical Center, Older patients, Medically unexplained symptoms, Health care, medicine, Humans, somatoform disorder, Psychiatry, Somatoform Disorders, Aged, Aged, 80 and over, Psychiatric Status Rating Scales, Health Services Needs and Demand, Primary Health Care, business.industry, Other Research Radboud Institute for Health Sciences [Radboudumc 0], Medically unexplained, Odds ratio, Middle Aged, medicine.disease, Confidence interval, Diagnostic and Statistical Manual of Mental Disorders, Psychiatry and Mental health, Case-Control Studies, Healthcare settings, psychiatric characteristics, Female, Symptom Assessment, business, Somatization, Stress, Psychological, Psychopathology, Research Article
Abstract

Background. Empirical studies on the clinical characteristics of older persons with medically unexplained symptoms are limited to uncontrolled pilot studies. Therefore, we aim to examine the psychiatric characteristics of older patients with medically unexplained symptoms (MUS) compared to older patients with medically explained symptoms (MES), also across healthcare settings. Methods. A case–control study including 118 older patients with MUS and 154 older patients with MES. To include patients with various developmental and severity stages, patients with MUS were recruited in the community (n = 12), primary care (n = 77), and specialized healthcare (n = 29). Psychopathology was assessed according to Diagnostic and Statistical Manual of Mental Disorders, Fourth Edition, Text Revision (DSM-IV-TR) criteria (Mini-International Neuropsychiatric Interview) and by dimensional measures (e.g., psychological distress, hypochondriasis, and depressive symptoms). Results. A total of 69/118 (58.5%) patients with MUS met the criteria for a somatoform disorder according to DSM-IV-TR criteria, with the highest proportion among patients recruited in specialized healthcare settings (p = 0.008). Patients with MUS had a higher level of psychological distress and hypochondriasis compared to patients with MES. Although psychiatric disorders (beyond somatoform disorders) were more frequently found among patients with MUS compared to patients with MES (42.4 vs. 24.8%, p = 0.008), this difference disappeared when adjusted for age, sex, and level of education (odds ratio = 1.7 [95% confidence interval: 1.0–3.0], p = 0.070). Conclusions. Although psychological distress is significantly higher among older patients with MUS compared to those with MES, psychiatric comorbidity rates hardly differ between both patient groups. Therefore, treatment of MUS in later life should primarily focus on reducing psychological distress, irrespective of the healthcare setting patients are treated in.

Published
2020

20. Assessment of Somatization and Medically Unexplained Symptoms in Later Life

Author

Peter H. Hilderink, T J W van Driel, P de Boer, Denise Hanssen, R.C. Oude Voshaar, Judith G. M. Rosmalen, Interdisciplinary Centre Psychopathology and Emotion regulation (ICPE), and Clinical Cognitive Neuropsychiatry Research Program (CCNP)

Subjects
Male, Psychometrics, Pilot Projects, Patient Health Questionnaire, 0302 clinical medicine, QUALITY-OF-LIFE, SOMATIC PERCEPTION QUESTIONNAIRE, Surveys and Questionnaires, somatic symptom disorders, Outpatients, 030212 general & internal medicine, somatic symptoms, PSYCHOLOGICAL DISTRESS, Applied Psychology, Aged, 80 and over, education.field_of_study, MUS, aged 80 years and older, Articles, somatoform disorders, Checklist, Clinical Psychology, aged, instruments, Female, Symptom Assessment, COMPLAINTS LIST GBB-24, Psychology, Clinical psychology, medicine.medical_specialty, PSYCHOMETRIC-PROPERTIES, Population, SELF-REPORT, 03 medical and health sciences, Quality of life (healthcare), Journal Article, medicine, Humans, OLDER-ADULTS, education, Psychiatry, GERIATRIC ANXIETY INVENTORY, Disease burden, Review study, Medically unexplained, Reproducibility of Results, PHYSICAL SYMPTOMS, medicine.disease, Medically Unexplained Symptoms, Somatization, 030217 neurology & neurosurgery
Abstract

The assessment of medically unexplained symptoms and “somatic symptom disorders” in older adults is challenging due to somatic multimorbidity, which threatens the validity of somatization questionnaires. In a systematic review study, the Patient Health Questionnaire–15 (PHQ-15) and the somatization subscale of the Symptom Checklist 90-item version (SCL-90 SOM) are recommended out of 40 questionnaires for usage in large-scale studies. While both scales measure physical symptoms which in younger persons often refer to unexplained symptoms, in older persons, these symptoms may originate from somatic diseases. Using empirical data, we show that PHQ-15 and SCL-90 SOM among older patients correlate with proxies of somatization as with somatic disease burden. Updating the previous systematic review, revealed six additional questionnaires. Cross-validation studies are needed as none of 46 identified scales met the criteria of suitability for an older population. Nonetheless, specific recommendations can be made for studying older persons, namely the SCL-90 SOM and PHQ-15 for population-based studies, the Freiburg Complaint List and somatization subscale of the Brief Symptom Inventory 53-item version for studies in primary care, and finally the Schedule for Evaluating Persistent Symptoms and Somatic Symptom Experiences Questionnaire for monitoring treatment studies.

Published
2017

21. A zone of avoidance catalogue of 2MASS bright galaxies – I. Sample description and analysis

Author

W. van Driel, Anke Schröder, R. C. Kraan-Korteweg, South African Astronomical Observatory (SAAO), Unité Scientifique de la Station de Nançay (USN), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université d'Orléans (UO), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), University of Cape Town, and Région Centre Val de Loire

Subjects
[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, infrared: galaxies, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 14. Life underwater, 010303 astronomy & astrophysics, Stellar density, Astrophysics::Galaxy Astrophysics, catalogues, Luminous infrared galaxy, Physics, [PHYS]Physics [physics], Extinction, 010308 nuclear & particles physics, Zone of Avoidance, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, galaxies: general, Redshift, Galaxy, Radial velocity, Stars, galaxies: photometry, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

We present a homogeneous 2MASS bright galaxy catalogue at low Galactic latitudes ($|b| \le 10.0^{\rm o}$, called Zone of Avoidance) which is complete to a Galactic extinction-corrected magnitude of $K^o_s \le 11.25^{\rm m}$. It also includes galaxies in regions of high foreground extinctions ($E(B-V) > 0.95^{\rm m}$) situated at higher latitudes. This catalogue forms the basis of studies of large-scale structures, flow fields and extinction across the ZoA and complements the ongoing 2MASS Redshift and Tully-Fisher surveys. It comprises 3763 galaxies, 70% of which have at least one radial velocity measurement in the literature. The catalogue is complete up to star density levels of $\log N_*/{\rm deg}^2, 29 pages, 16 figures; accepted for publication in MNRAS; full catalogue available as ancillary file in sourcefile package

Published
2019

22. The WSRT ZoA Perseus-Pisces filament wide-field H I imaging survey - I. H I catalogue and atlas

Author

M. Ramatsoku, Edward C. Elson, Anke Schröder, W. J. G. de Blok, Marc Verheijen, Gyula I. G. Józsa, P. A. Henning, W. van Driel, R. C. Kraan-Korteweg, Thomas H. Jarrett, and Astronomy

Subjects
AVOIDANCE SURVEY, Radio galaxy, Milky Way, BACKGROUND DIPOLE, DATA RELEASE, 2MASS REDSHIFT SURVEY, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, GALACTIC PLANE, surveys, Supercluster, 0103 physical sciences, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, catalogues, LOCAL UNIVERSE, Physics, radio lines: galaxies, 010308 nuclear & particles physics, Astronomy, Velocity dispersion, Astronomy and Astrophysics, PECULIAR VELOCITY, Galactic plane, Redshift survey, Astrophysics - Astrophysics of Galaxies, DENSITY FIELD, Galaxy, atlases, Space and Planetary Science, galaxies: clusters: general, Astrophysics of Galaxies (astro-ph.GA), MILKY-WAY, GALAXY CLUSTERS
Abstract

We present results of a blind 21cm HI-line imaging survey of a galaxy overdensity located behind the Milky Way at $\ell,b$ $\approx$ 160 deg, 0.5 deg. The overdensity corresponds to a Zone-of-Avoidance crossing of the Perseus-Pisces Supercluster filament. Although it is known that this filament contains an X-ray galaxy cluster (3C129) hosting two strong radio galaxies, little is known about galaxies associated with this potentially rich cluster because of the high Galactic dust extinction. We mapped a sky area of $\sim$9.6 sq.deg using the Westerbork Synthesis Radio Telescope in a hexagonal mosaic of 35 pointings observed for 12 hours each, in the radial velocity range $cz = 2400 - 16600$ km/s. The survey has a sensitivity of 0.36 mJy/beam rms at a velocity resolution of 16.5 km/s. We detected 211 galaxies, 62% of which have a near-infrared counterpart in the UKIDSS Galactic Plane Survey. We present a catalogue of the HI properties and an HI atlas containing total intensity maps, position-velocity diagrams, global HI profiles and UKIDSS counterpart images. For the resolved galaxies we also present HI velocity fields and radial HI surface density profiles. A brief analysis of the structures outlined by these galaxies finds that 87 of them lie at the distance of the Perseus-Pisces Supercluster ($cz \sim 4000 - 8000$ km/s) and seem to form part of the 3C129 cluster. Further 72 detections trace an overdensity at a velocity of $cz \approx$ 10000 km/s and seem to coincide with a structure predicted from mass density reconstructions in the first 2MASS Redshift Survey., 28 pages, 18 figures, 6 Tables, accepted for publication in MNRAS

Published
2016

24. Bivariate luminosity-HI mass distribution function of galaxies based on the NIBLES survey

Author

Matt Lehnert, Stephen E. Schneider, W. van Driel, Z. Butcher, University of Massachusetts [Amherst] (UMass Amherst), University of Massachusetts System (UMASS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Unité Scientifique de la Station de Nançay (USN), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and Région Centre Val de Loire - France

Subjects
media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, symbols.namesake, 0103 physical sciences, Range (statistics), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Line (formation), Luminosity function (astronomy), Physics, radio lines: galaxies, Mass distribution, 010308 nuclear & particles physics, Astronomy and Astrophysics, galaxies: fundamental parameters, galaxies: general, Astrophysics - Astrophysics of Galaxies, Universe, Galaxy, galaxies: luminosity function, Space and Planetary Science, mass function, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), symbols, galaxies: distances and redshifts, galaxies: evolution, Hubble's law
Abstract

We present a new optical luminosity-HI mass bivariate luminosity function (BLF) based on HI line observations from the Nancay Interstellar Baryons Legacy Extragalactic Survey (NIBLES). NIBLES sources lie within the local universe (900 $\leq cz \leq$ 12,000 \kms) and were chosen from SDSS DR5 such that the optical luminosity function was sampled as uniformly as possible. The HI mass function (HIMF) derived from our raw-data BLF, which is based on HI detections only, is consistent with the HIMFs derived from other optically selected surveys in that the low-mass slope is flatter than those derived from blind HI surveys. However, spanning the entire luminosity range of NIBLES, we identify a highly consistent distribution of the HI gas mass to luminosity ratio (gas-to-light ratio) with a predictable progression in the mean MHI/Lr ratio as a function of Lr. This consistency allows us to construct plausible gas-to-light ratio distributions for very low-luminosity bins which lie outside the NIBLES sample. We also identify a $\sim$ 10% decrease in detection fraction for galaxies fainter than log(\Lr) = 9.25, consistent with the expected decrease due to distance and sensitivity effects. Accounting for these trends, we reconstruct plausible gas-to-light distributions spanning luminosity bins down to log(\Lr) = 5.25, thus producing a corrected BLF. This corrected BLF is in good qualitative agreement with optical luminosity-HI mass distributions from the ALFALFA survey and is able to accurately reproduce blind survey HIMFs, lending credibility that this two dimensional optical luminosity-HI mass distribution is an accurate representation of the volume density distribution of galaxies in the local universe. We also note that our agreement with HIMFs from other surveys is dependent on accounting for all systematic differences such as selection method, Hubble constant and HI flux scale., 15 pages, 14 figures

Published
2018

25. A study of the HI and optical properties of Low Surface Brightness galaxies: spirals, dwarfs and irregulars

Author

W. van Driel, M Honey, Mousumi Das, J. M. Martin, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
galaxies: spiral, Brightness, Stellar mass, Star (game theory), Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Surface brightness, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, radio lines: galaxies, [PHYS]Physics [physics], Physics, education.field_of_study, 010308 nuclear & particles physics, Astronomy and Astrophysics, galaxies: general, Astrophysics - Astrophysics of Galaxies, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Magnitude (astronomy), galaxies: structure, Local environment, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

We present a study of the HI and optical properties of nearby ($z$ $\le$ 0.1) Low Surface Brightness galaxies (LSBGs). We started with a literature sample of $\sim$900 LSBGs and divided them into three morphological classes: spirals, irregulars and dwarfs. Of these, we could use $\sim$490 LSBGs to study their HI and stellar masses, colours and colour magnitude diagrams, and local environment, compare them with normal, High Surface Brightness (HSB) galaxies and determine the differences between the three morphological classes. We found that LSB and HSB galaxies span a similar range in HI and stellar masses, and have a similar $M_{\rm HI}$/$M_{\star}$--$M_{\star}$ relationship. Among the LSBGs, as expected, the spirals have the highest average HI and stellar masses, both of about 10$^{9.8}$ $M_\odot$. The LSGBs' ($g$--$r$) integrated colour is nearly constant as function of HI mass for all classes. In the colour magnitude diagram, the spirals are spread over the red and blue regions whereas the irregulars and dwarfs are confined to the blue region. The spirals also exhibit a steeper slope in the $M_{\rm HI}$/$M_{\star}$--$M_{\star}$ plane. Within their local environment we confirmed that LSBGs are more isolated than HSB galaxies, and LSB spirals more isolated than irregulars and dwarfs. Kolmogorov-Smirnov statistical tests on the HI mass, stellar mass and number of neighbours indicates that the spirals are a statistically different population from the dwarfs and irregulars. This suggests that the spirals may have different formation and HI evolution than the dwarfs and irregulars., 37 pages, 9 figures, Accepted for publication in MNRAS

Published
2018

26. The LOFAR Two-metre Sky Survey: I. Survey description and preliminary data release

Author

Jeremy J. Harwood, Matthias Steinmetz, W. van Driel, Leah K. Morabito, Emanuela Orru, Magdalena Kunert-Bajraszewska, D. A. Rafferty, Isabella Prandoni, A. Horneffer, Huub Röttgering, R. J. van Weeren, Adam Deller, Subhash C. Mandal, J. Sabater, G. Calistro Rivera, M. Sipior, Daniel J. Smith, Frank P. Israel, Aleksandar Shulevski, John McKean, Marijke Haverkorn, D. Engels, Krzysztof T. Chyzy, Chiara Ferrari, P. van der Werf, Philip Best, J. B. R. Oonk, A. Drabent, Elizabeth K. Mahony, Raffaella Morganti, Marisa Brienza, Timothy W. Shimwell, Michael W. Wise, Annalisa Bonafede, Martin J. Hardcastle, Rainer Beck, S. S. Sridhar, Marcus Brüggen, Neal Jackson, Dominik J. Schwarz, M. A. Garrett, Cathy Horellou, Matthias Hoeft, J. A. Zensus, Gianfranco Brunetti, N. R. Mohan, George K. Miley, Andra Stroe, John Conway, Anna D. Kapińska, E. Retana-Montenegro, D. J. McKay, A. O. Clarke, I. van Bemmel, Glenn J. White, George Heald, Volker Heesen, Heino Falcke, Matt J. Jarvis, F. de Gasperin, Huib Intema, D. N. Hoang, Cyril Tasse, R. Pizzo, Eskil Varenius, S. Fröhlich, A. P. Mechev, D. Cseh, Wendy L. Williams, Rossella Cassano, Jonathan T. L. Zwart, T. J. Dijkema, Leiden Observatory [Leiden], Universiteit Leiden, Institute for Astronomy [Edinburgh] (IfA), University of Edinburgh, Centre for Astrophysics Research, University of Hertfordshire [Hatfield] (UH), Netherlands Institute for Radio Astronomy (ASTRON), Hamburger Sternwarte/Hamburg Observatory, Universität Hamburg (UHH), Max-Planck-Institut für Radioastronomie (MPIFR), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, Istituto di Radioastronomia [Bologna] (IRA), Istituto Nazionale di Astrofisica (INAF), Astronomical Observatory [Kraków], Uniwersytet Jagielloński w Krakowie = Jagiellonian University (UJ), Onsala Space Observatory (OSO), Chalmers University of Technology [Göteborg], Radboud University [Nijmegen], Jodrell Bank Centre for Astrophysics, University of Manchester [Manchester], Oxford Astrophysics, University of Oxford, Department of Physics and Astronomy [Milton Keynes], The Open University [Milton Keynes] (OU), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Thüringer Landessternwarte Tautenburg (TLS), Unité Scientifique de la Station de Nançay (USN), Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Institute for Mathematics, Astrophysics and Particle Physics (IMAPP), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Ruhr-Universität Bochum [Bochum], School of Physics and Astronomy [Southampton], University of Southampton, Joint Institute for VLBI in Europe (JIVE ERIC), Department of Earth and Space Sciences [Göteborg], The University of Western Australia (UWA), Torun Centre for Astronomy (TCfA), Nicolaus Copernicus University [Toruń], University of Oulu, National Centre for Radio Astrophysics [Pune] (NCRA), Tata Institute for Fundamental Research (TIFR), Universität Bielefeld, Leibniz-Institut für Astrophysik Potsdam (AIP), European Southern Observatory (ESO), University of the Western Cape (UWC), European Project: 320745,EC:FP7:ERC,ERC-2012-ADG_20120216,RADIOLIFE(2013), Astronomy, Kapteyn Astronomical Institute, Universiteit Leiden [Leiden], Harvard University [Cambridge]-Smithsonian Institution, Radboud university [Nijmegen], University of Oxford [Oxford], Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of the Western Cape, High Energy Astrophys. & Astropart. Phys (API, FNWI), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Smithsonian Institution-Harvard University [Cambridge], Istituto di Radioastronomia INAF, Jagiellonian University [Krakow] (UJ), Onsala Space Observatory, Istituto di Radioastronomia (IRA), Université d'Orléans (UO)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), and Tata Institute of Fundamental Research [Bombay] (TIFR)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, media_common.quotation_subject, Astronomy, radio continuum: general, FOS: Physical sciences, techniques: image processing, 01 natural sciences, Declination, Spectral line, RADIO RECOMBINATION LINES, techniques image processing, surveys, CALIBRATOR SURVEY, 0103 physical sciences, Calibration, radio-continuum, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Remote sensing, media_common, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], image processing [techniques], QUASAR SURVEY, Astronomy and Astrophysics, HERSCHEL-ATLAS, LOFAR, 1ST SURVEY, Galaxy, WIDE-FIELD, Space and Planetary Science, Sky, LUMINOSITY FUNCTION, general, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, general [radio continuum], CHANDRA OBSERVATIONS, Astrophysics - Instrumentation and Methods for Astrophysics, Right ascension, FOLLOW-UP, GALAXY CLUSTERS, surveys – catalogs – radio continuum: general – techniques: image processing, Geology, Noise (radio), catalogs, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The LOFAR Two-metre Sky Survey (LoTSS) is a deep 120-168 MHz imaging survey that will eventually cover the entire Northern sky. Each of the 3170 pointings will be observed for 8 hrs, which, at most declinations, is sufficient to produce ~5arcsec resolution images with a sensitivity of ~0.1mJy/beam and accomplish the main scientific aims of the survey which are to explore the formation and evolution of massive black holes, galaxies, clusters of galaxies and large-scale structure. Due to the compact core and long baselines of LOFAR, the images provide excellent sensitivity to both highly extended and compact emission. For legacy value, the data are archived at high spectral and time resolution to facilitate subarcsecond imaging and spectral line studies. In this paper we provide an overview of the LoTSS. We outline the survey strategy, the observational status, the current calibration techniques, a preliminary data release, and the anticipated scientific impact. The preliminary images that we have released were created using a fully-automated but direction-independent calibration strategy and are significantly more sensitive than those produced by any existing large-area low-frequency survey. In excess of 44,000 sources are detected in the images that have a resolution of 25arcsec, typical noise levels of less than 0.5 mJy/beam, and cover an area of over 350 square degrees in the region of the HETDEX Spring Field (right ascension 10h45m00s to 15h30m00s and declination 45d00m00s to 57d00m00s)., Comment: 23 pages, 15 figures, 3 tables, accepted for publication in A&A

Published
2017

27. Prospects for Cherenkov Telescope Array Observations of the Young Supernova Remnant RX J1713.7−3946

Author

Csaba Balázs, M. Servillat, F. D'Ammando, D. Nosek, T. Yamamoto, A. Bilinsky, H.-S. Zechlin, Francesco Dazzi, A. Fernández-Barral, Satoshi Yoshiike, Catherine Boisson, Philippe Laporte, K. Nishijima, Yutaka Fujita, T. Armstrong, A. Shalchi, S. Kimura, D. Nakajima, Fuyuki Tokanai, Francesco Longo, S. Pavy, Philip Kaaret, W. van Driel, Gianpiero Tagliaferri, L. Nogués, F. Di Pierro, Wystan Benbow, T. Stolarczyk, Marco Padovani, T. Di Girolamo, Johan Bregeon, J. Rico, R. Wischnewski, A. Sillanpää, T. Grabarczyk, E. Pueschel, P. Blasi, S. D. Vergani, A. De Franco, C. Bonavolontà, J. Prast, J. Zorn, Elisabetta Bissaldi, Giuseppe Malaguti, A. Pe'Er, Stefano Covino, Akira Okumura, Takashi Saito, C. Aramo, Hermine Landt, R. Zanin, E. Fedorova, Shinji Hara, Yutaka Ohira, Petr Janecek, Petar Temnikov, T. B. Humensky, E. Fiandrini, C. Townsley, R. J. White, A. Fiasson, Koji Noda, Takanori Yoshikoshi, Y. Ikeno, Elena Amato, Yasuo Fukui, J. P. Lees, M. Nievas-Rosillo, Vito Conforti, Kazunori Kohri, I. Oya, M. Trifoglio, Gavin Rowell, Jacek Niemiec, Juan Abel Barrio, R. Walter, Stefan Wagner, Teresa Mineo, J. J. Watson, Reiko Orito, Masahiro Teshima, Jim Hinton, A. Pisarski, G. Rodriguez Fernandez, F. De Frondat, Robert Wagner, Pedro L. Luque-Escamilla, G. Morlino, Thomas Lohse, B. Rudak, Olaf Reimer, Josep Martí, Subir Sarkar, Martin White, Johann Cohen-Tanugi, Michiyuki Chikawa, Dusan Mandat, T. Montaruli, M. Mohammed, M. Iori, Oscar Blanch, Giovanni Bonanno, Benjamin Koch, M. A. Lopez, Julien Rousselle, M. Heller, Yusuke Konno, G. Maurin, J. Palacio, S. Gunji, C. Di Giulio, M. Zavrtanik, J.-P. Lenain, Adrian Biland, Michael Backes, Miroslav Filipovic, M. I. Martínez, M. Vazquez Acosta, Nicola Giglietto, J. M. Paredes, G. Fontaine, R. Moderski, A.A. Zdziarski, D. Tescaro, V. Vassiliev, C. van Eldik, H. Siejkowski, Stefan Kimeswenger, Shu Koyama, A. Bonardi, R. Gnatyk, S. Vorobiov, Oleh Petruk, M. Del Santo, Michał Szanecki, C. Delgado, Carole Mundell, Tomasz Szepieniec, Michael G. Burton, Bohdan Hnatyk, M. Capalbi, Kunihito Ioka, Jonathan Granot, Bohdan Novosyadlyj, Petr Schovanek, A. Weinstein, M. Stephan, Vikram V. Dwarkadas, L. Valore, Sabrina Einecke, P. Goldoni, J. Jacquemier, Hiroshi Muraishi, Andreas Quirrenbach, Takeshi Nakamori, Stefan Ohm, G. Busetto, Marcos Santander, A. Wierzcholska, Jaime Rosado, M. Yoshida, M. Huetten, S. Eschbach, Tatsuo Yoshida, Tomasz Bulik, Gino Tosti, Valentina Fioretti, Makoto Sawada, D. Zavrtanik, P. A. Caraveo, Mohamed Rameez, Sylvain Chaty, Nu. Komin, D. Dumas, Michael Zacharias, J. M. Huet, Reshmi Mukherjee, F. Lucarelli, L. Di Venere, Shuta J. Tanaka, F. de Palma, Shiu-Hang Lee, A. W. Chen, A. Giuliani, R. L. C. Starling, V. Beshley, Jonathan S. Lapington, Gilles Ferrand, Giovanni Covone, Rodrigo Nemmen, Tsuyoshi Inoue, R. C. Shellard, P. Cumani, G. Lamanna, Stefan Funk, Michele Doro, Koji Mori, G. Pühlhofer, Hidetoshi Sano, Susumu Inoue, Luis Ángel Tejedor, G. Kukec Mezek, Anderson Caproni, L. Freixas Coromina, M. de Naurois, D. Jankowsky, Yoshiyuki Inoue, Elina Lindfors, Saverio Lombardi, D. della Volpe, Giancarlo Cusumano, Andrea Orlati, S. Mangano, Samar Safi-Harb, Alexandre Marcowith, R. López-Coto, Martin Pohl, J. Lefaucheur, Vincenzo Rizi, Masayuki Tanaka, Shigehiro Nagataki, J. L. Rodriguez, Diego Falceta-Gonçalves, J. E. Ward, Petr Travnicek, I. Sadeh, Dominik Elsässer, P. Wilcox, Tsunefumi Mizuno, Kohta Murase, K. Lalik, M. Ostrowski, Vincenzo Testa, Tsuguya Naito, Matteo Cerruti, N. La Palombara, Yukikatsu Terada, Emmanuel Moulin, A. Balzer, M. Palatka, Samo Stanič, D. D'Urso, Łukasz Stawarz, D. Simone, Giuseppe Romeo, Francesco Giordano, Luca Zampieri, Michiko Ohishi, Giuseppe Leto, J.F. Glicenstein, G. De Cesare, Eleonora Torresi, R. A. Cameron, Katsuaki Asano, Ricardo Graciani, Gernot Maier, Paweł Wójcik, R. A. Ong, Jörg R. Hörandel, Carlo Vigorito, S. P. Wakely, Valerio Vagelli, Andrea Bulgarelli, J. Takeda, S. Brau-Nogué, Garret Cotter, Claudio Melioli, Hiroaki Yamamoto, M. Vrastil, Ryo Yamazaki, G. Maneva, N. Maxted, David A. Williams, K. Kosack, Konrad Bernlöhr, Markus Böttcher, Andreas Zech, Jürgen Knödlseder, Daniel Nieto, Paola Grandi, Maria Concetta Maccarone, Y. Inome, I. Telezhinsky, Fabio Acero, Michael C. B. Ashley, D. A. Sanchez, C. de Lisio, Francisco J. Franco, J. L. Dournaux, M. Kraus, G. Bonnoli, Xian Chen, Massimo Persic, Jonathan Blazek, Giacomo Principe, Louis Antonelli, H. Hakobyan, A. De Angelis, Marek Nikolajuk, F. Schüssler, T. Nagayoshi, P.-O. Petrucci, P. Sangiorgi, N. Sakaki, Anthony M. Brown, S. Tsujimoto, J. J. Rodríguez Vázquez, A. Morselli, B. De Lotto, Juan Carlos Helo, S. Nozaki, M. Takahashi, Lili Yang, H. Schoorlemmer, Catherine Braiding, Justin Vandenbroucke, J. A. Graham, P. Vallania, Stanislav Stefanik, M. Fesquet, Roberto Aloisio, Diego F. Torres, Ciro Bigongiari, C. Díaz, Shohei Yanagita, M. Garczarczyk, Abelardo Moralejo, Hideaki Katagiri, R. de los Reyes Lopez, A. Burtovoi, M. Hussein, Hiroyasu Tajima, M. Prouza, M. Renaud, C. Trichard, M. K. Daniel, Maria Chernyakova, Tarek M. Hassan, A. Ziegler, E. M. de Gouveia Dal Pino, Ll. Font, J. Kocot, Jiri Chudoba, J. P. Amans, Enrico Junior Schioppa, Alessandro Costa, Aya Bamba, A. Förster, F. Arqueros, Jan Ebr, M. Hayashida, A. J. Green, Marc Ribó, Olga Sergijenko, Hidetoshi Kubo, A. Porcelli, Tomohiro Inada, J. Biteau, J. Kushida, Jose Luis Contreras, S. Colafrancesco, Nestor Mirabal, V. Bugaev, R. J. García López, Vitalii Sliusar, I. Jung, Kathrin Egberts, G. Fasola, Maxim V. Barkov, Seiji Masuda, P. Romano, Enrico Cascone, V. I. Zhdanov, Elisa Prandini, Helene Sol, Rodolfo Carosi, S. Vercellone, Manuela Vecchi, German Martinez, A. Gadola, S. Griffiths, Satyendra Thoudam, Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Institut de Physique Nucléaire d'Orsay (IPNO), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPP), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), CTA Consortium, High Energy Astrophys. & Astropart. Phys (API, FNWI), Acero F., Aloisio R., Amans J., Amato E., Antonelli L. A., Aramo C., Armstrong T., Arqueros F., Asano K., Ashley M., Backes M., Balazs C., Balzer A., Bamba A., Barkov M., Barrio J. A., Benbow W., Bernlöhr K., Beshley V., Bigongiari C., Biland A., Bilinsky A., Bissaldi E., Biteau J., Blanch O., Blasi P., Blazek J., Boisson C., Bonanno G., Bonardi A., Bonavolontà C., Bonnoli G., Braiding C., Brau-Nogué S., Bregeon J., Brown A. M., Bugaev V., Bulgarelli A., Bulik T., Burton M., Burtovoi A., Busetto G., Böttcher M., Cameron R., Capalbi M., Caproni A., Caraveo P., Carosi R., Cascone E., Cerruti M., Chaty S., Chen A., Chen X., Chernyakova M., Chikawa M., Chudoba J., Cohen-Tanugi J., Colafrancesco S., Conforti V., Contreras J. L., Costa A., Cotter G., Covino S., Covone G., Cumani P., Cusumano G., D’Ammando F., D’Urso D., Daniel M., Dazzi F., De Angelis A., De Cesare G., De Franco A., De Frondat F., de Gouveia Dal Pino E. M., De Lisio C., de los Reyes Lopez R., De Lotto B., de Naurois M., De Palma F., Del Santo M., Delgado C., della Volpe D., Di Girolamo T., Di Giulio C., Di Pierro F., Di Venere L., Doro M., Dournaux J., Dumas D., Dwarkadas V., Díaz C., Ebr J., Egberts K., Einecke S., Elsässer D., Eschbach S., Falceta-Goncalves D., Fasola G., Fedorova E., Fernández-Barral A., Ferrand G., Fesquet M., Fiandrini E., Fiasson A., Filipovíc M. D., Fioretti V., Font L., Fontaine G., Franco F. J., Coromina L. Freixa, Fujita Y., Fukui Y., Funk S., Förster A., Gadola A., López R. Garcia, Garczarczyk M., Giglietto N., Giordano F., Giuliani A., Glicenstein J., Gnatyk R., Goldoni P., Grabarczyk T., Graciani R., Graham J., Grandi P., Granot J., Green A. J., Griffiths S., Gunji S., Hakobyan H., Hara S., Hassan T., Hayashida M., Heller M., Helo J. C., Hinton J., Hnatyk B., Huet J., Huetten M., Humensky T. B., Hussein M., Hörandel J., Ikeno Y., Inada T., Inome Y., Inoue S., Inoue T., Inoue Y., Ioka K., Iori M., Jacquemier J., Janecek P., Jankowsky D., Jung I., Kaaret P., Katagiri H., Kimeswenger S., Kimura S., Knödlseder J., Koch B., Kocot J., Kohri K., Komin N., Konno Y., Kosack K., Koyama S., Kraus M., Kubo H., Mezek G. Kukec, Kushida J., Palombara N. La, Lalik K., Lamanna G., Landt H., Lapington J., Laporte P., Lee S., Lees J., Lefaucheur J., Lenain J.-P., Leto G., Lindfors E., Lohse T., Lombardi S., Longo F., Lopez M., Lucarelli F., Luque-Escamilla P. L., López-Coto R., Maccarone M. C., Maier G., Malaguti G., Mandat D., Maneva G., Mangano S., Marcowith A., Martí J., Martínez M., Martínez G., Masuda S., Maurin G., Maxted N., Melioli C., Mineo T., Mirabal N., Mizuno T., Moderski R., Mohammed M., Montaruli T., Moralejo A., Mori K., Morlino G., Morselli A., Moulin E., Mukherjee R., Mundell C., Muraishi H., Murase K., Nagataki S., Nagayoshi T., Naito T., Nakajima D., Nakamori T., Nemmen R., Niemiec J., Nieto D., Nievas-Rosillo M., Nikołajuk M., Nishijima K., Noda K., Nogues L., Nosek D., Novosyadlyj B., Nozaki S., Ohira Y., Ohishi M., Ohm S., Okumura A., Ong R. A., Orito R., Orlati A., Ostrowski M., Oya I., Padovani M., Palacio J., Palatka M., Paredes J. M., Pavy S., Pe’Er A., Persic M., Petrucci P., Petruk O., Pisarski A., Pohl M., Porcelli A., Prandini E., Prast J., Principe G., Prouza M., Pueschel E., Pühlhofer G., Quirrenbach A., Rameez M., Reimer O., Renaud M., Ribó M., Rico J., Rizi V., Rodriguez J., Fernandez G. Rodriguez, Vázquez J. J. Rodríguez, Romano P., Romeo G., Rosado J., Rousselle J., Rowell G., Rudak B., Sadeh I., Safi-Harb S., Saito T., Sakaki N., Sanchez D., Sangiorgi P., Sano H., Santander M., Sarkar S., Sawada M., Schioppa E. J., Schoorlemmer H., Schovanek P., Schussler F., Sergijenko O., Servillat M., Shalchi A., Shellard R. C., Siejkowski H., Sillanpää A., Simone D., Sliusar V., Sol H., Stanič S., Starling R., Stawarz Ł., Stefanik S., Stephan M., Stolarczyk T., Szanecki M., Szepieniec T., Tagliaferri G., Tajima H., Takahashi M., Takeda J., Tanaka M., Tanaka S., Tejedor L. A., Telezhinsky I., Temnikov P., Terada Y., Tescaro D., Teshima M., Testa V., Thoudam S., Tokanai F., Torres D. F., Torresi E., Tosti G., Townsley C., Travnicek P., Trichard C., Trifoglio M., Tsujimoto S., Vagelli V., Vallania P., Valore L., van Driel W., van Eldik C., Vandenbroucke J., Vassiliev V., Vecchi M., Vercellone S., Vergani S., Vigorito C., Vorobiov S., Vrastil M., Acosta M. L. Vázquez, Wagner S. J., Wagner R., Wakely S. P., Walter R., Ward J. E., Watson J. J., Weinstein A., White M., White R., Wierzcholska A., Wilcox P., Williams D. A., Wischnewski R., Wojcik P., Yamamoto T., Yamamoto H., Yamazaki R., Yanagita S., Yang L., Yoshida T., Yoshida M., Yoshiike S., Yoshikoshi T., Zacharias M., Zampieri L., Zanin R., Zavrtanik M., Zavrtanik D., Zdziarski A., Zech A., Zechlin H., Zhdanov V., Ziegler A., Zorn J., Acero, F., Aloisio, R., Amans, J., Amato, E., Antonelli, L. A., Aramo, C., Armstrong, T., Arqueros, F., Asano, K., Ashley, M., Backes, M., Balazs, C., Balzer, A., Bamba, A., Barkov, M., Barrio, J. A., Benbow, W., Bernlöhr, K., Beshley, V., Bigongiari, C., Biland, A., Bilinsky, A., Bissaldi, E., Biteau, J., Blanch, O., Blasi, P., Blazek, J., Boisson, C., Bonanno, G., Bonardi, A., Bonavolontà, C., Bonnoli, G., Braiding, C., Brau Nogué, S., Bregeon, J., Brown, A. M., Bugaev, V., Bulgarelli, A., Bulik, T., Burton, M., Burtovoi, A., Busetto, G., Böttcher, M., Cameron, R., Capalbi, M., Caproni, A., Caraveo, P., Carosi, R., Cascone, E., Cerruti, M., Chaty, S., Chen, A., Chen, X., Chernyakova, M., Chikawa, M., Chudoba, J., Cohen Tanugi, J., Colafrancesco, S., Conforti, V., Contreras, J. L., Costa, A., Cotter, G., Covino, S., Covone, G., Cumani, P., Cusumano, G., D’Ammando, F., D’Urso, D., Daniel, M., Dazzi, F., De Angelis, A., De Cesare, G., De Franco, A., De Frondat, F., de Gouveia Dal Pino, E. M., De Lisio, C., de los Reyes Lopez, R., De Lotto, B., de Naurois, M., De Palma, F., Del Santo, M., Delgado, C., della Volpe, D., Di Girolamo, T., Di Giulio, C., Di Pierro, F., Di Venere, L., Doro, M., Dournaux, J., Dumas, D., Dwarkadas, V., Díaz, C., Ebr, J., Egberts, K., Einecke, S., Elsässer, D., Eschbach, S., Falceta Goncalves, D., Fasola, G., Fedorova, E., Fernández Barral, A., Ferrand, G., Fesquet, M., Fiandrini, E., Fiasson, A., Filipovíc, M. D., Fioretti, V., Font, L., Fontaine, G., Franco, F. J., Coromina, L. Freixa, Fujita, Y., Fukui, Y., Funk, S., Förster, A., Gadola, A., López, R. Garcia, Garczarczyk, M., Giglietto, N., Giordano, F., Giuliani, A., Glicenstein, J., Gnatyk, R., Goldoni, P., Grabarczyk, T., Graciani, R., Graham, J., Grandi, P., Granot, J., Green, A. J., Griffiths, S., Gunji, S., Hakobyan, H., Hara, S., Hassan, T., Hayashida, M., Heller, M., Helo, J. C., Hinton, J., Hnatyk, B., Huet, J., Huetten, M., Humensky, T. B., Hussein, M., Hörandel, J., Ikeno, Y., Inada, T., Inome, Y., Inoue, S., Inoue, T., Inoue, Y., Ioka, K., Iori, M., Jacquemier, J., Janecek, P., Jankowsky, D., Jung, I., Kaaret, P., Katagiri, H., Kimeswenger, S., Kimura, S., Knödlseder, J., Koch, B., Kocot, J., Kohri, K., Komin, N., Konno, Y., Kosack, K., Koyama, S., Kraus, M., Kubo, H., Mezek, G. Kukec, Kushida, J., Palombara, N. La, Lalik, K., Lamanna, G., Landt, H., Lapington, J., Laporte, P., Lee, S., Lees, J., Lefaucheur, J., Lenain, J. P., Leto, G., Lindfors, E., Lohse, T., Lombardi, S., Longo, Francesco, Lopez, M., Lucarelli, F., Luque Escamilla, P. L., López Coto, R., Maccarone, M. C., Maier, G., Malaguti, G., Mandat, D., Maneva, G., Mangano, S., Marcowith, A., Martí, J., Martínez, M., Martínez, G., Masuda, S., Maurin, G., Maxted, N., Melioli, C., Mineo, T., Mirabal, N., Mizuno, T., Moderski, R., Mohammed, M., Montaruli, T., Moralejo, A., Mori, K., Morlino, G., Morselli, A., Moulin, E., Mukherjee, R., Mundell, C., Muraishi, H., Murase, K., Nagataki, S., Nagayoshi, T., Naito, T., Nakajima, D., Nakamori, T., Nemmen, R., Niemiec, J., Nieto, D., Nievas Rosillo, M., Nikołajuk, M., Nishijima, K., Noda, K., Nogues, L., Nosek, D., Novosyadlyj, B., Nozaki, S., Ohira, Y., Ohishi, M., Ohm, S., Okumura, A., Ong, R. A., Orito, R., Orlati, A., Ostrowski, M., Oya, I., Padovani, M., Palacio, J., Palatka, M., Paredes, J. M., Pavy, S., Pe’Er, A., Persic, M., Petrucci, P., Petruk, O., Pisarski, A., Pohl, M., Porcelli, A., Prandini, E., Prast, J., Principe, G., Prouza, M., Pueschel, E., Pühlhofer, G., Quirrenbach, A., Rameez, M., Reimer, O., Renaud, M., Ribó, M., Rico, J., Rizi, V., Rodriguez, J., Fernandez, G. Rodriguez, Vázquez, J. J. Rodríguez, Romano, P., Romeo, G., Rosado, J., Rousselle, J., Rowell, G., Rudak, B., Sadeh, I., Safi Harb, S., Saito, T., Sakaki, N., Sanchez, D., Sangiorgi, P., Sano, H., Santander, M., Sarkar, S., Sawada, M., Schioppa, E. J., Schoorlemmer, H., Schovanek, P., Schussler, F., Sergijenko, O., Servillat, M., Shalchi, A., Shellard, R. C., Siejkowski, H., Sillanpää, A., Simone, D., Sliusar, V., Sol, H., Stanič, S., Starling, R., Stawarz, Ł., Stefanik, S., Stephan, M., Stolarczyk, T., Szanecki, M., Szepieniec, T., Tagliaferri, G., Tajima, H., Takahashi, M., Takeda, J., Tanaka, M., Tanaka, S., Tejedor, L. A., Telezhinsky, I., Temnikov, P., Terada, Y., Tescaro, D., Teshima, M., Testa, V., Thoudam, S., Tokanai, F., Torres, D. F., Torresi, E., Tosti, G., Townsley, C., Travnicek, P., Trichard, C., Trifoglio, M., Tsujimoto, S., Vagelli, V., Vallania, P., Valore, L., van Driel, W., van Eldik, C., Vandenbroucke, J., Vassiliev, V., Vecchi, M., Vercellone, S., Vergani, S., Vigorito, C., Vorobiov, S., Vrastil, M., Acosta, M. L. Vázquez, Wagner, S. J., Wagner, R., Wakely, S. P., Walter, R., Ward, J. E., Watson, J. J., Weinstein, A., White, M., White, R., Wierzcholska, A., Wilcox, P., Williams, D. A., Wischnewski, R., Wojcik, P., Yamamoto, T., Yamamoto, H., Yamazaki, R., Yanagita, S., Yang, L., Yoshida, T., Yoshida, M., Yoshiike, S., Yoshikoshi, T., Zacharias, M., Zampieri, L., Zanin, R., Zavrtanik, M., Zavrtanik, D., Zdziarski, A., Zech, A., Zechlin, H., Zhdanov, V., Ziegler, A., Zorn, J., Acero et al, F., PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Centre National de la Recherche Scientifique (CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPhP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Acero, F, Aloisio, R, Amans, J, De Lisio, C, Di Girolamo, T, Valore, L, Covone, G, and Al., Et

Subjects
electron, Supernova Remnants, PARTICLE-ACCELERATION, Cherenkov Telescope Array, Astronomy, leptonic, Telescope Array Experiment, pi, Astrophysics, 01 natural sciences, Supernova Remnant, LARGE-AREA TELESCOPE, Spectral line, spectrum, ISM: individual objects, HESS, Supernova remnant, 010303 astronomy & astrophysics, cosmic ray, Physics, cosmic rays gamma rays: ISM ISM: individual objects (RX J1713.7-3946, G347.3-0.5), spatial distribution, Gamma Ray, Cherenkov radiation, MAGNETIC-FIELD, Gamma ray, COSMIC-RAYS, ISM: individual objects (RX J1713.7–3946, G347.3–0.5), Supernova, cosmic rays, gamma rays: ISM, ISM: individual objects (RX J1713.7-3946, G347.3-0.5), Astronomy and Astrophysics, Space and Planetary Science, gamma ray: emission, G347.3–0.5, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, DIFFUSIVE SHOCK ACCELERATION, Electrónica, Física nuclear, Electricidad, individual objects: RX J1713.7–3946 [ISM], Compton scattering, Gamma Rays, G347.3-0.5), NONTHERMAL, accelerator, X-RAYS, Astrophysics::High Energy Astrophysical Phenomena, INSTABILITY, Cosmic ray, hadronic, GLAST, ISM: individual objects (RX J1713.7-3946, ISM [gamma rays], gas, 0103 physical sciences, supernova, ddc:530, X-ray: emission, GAMMA-RAY EMISSION, AMPLIFICATION, BROAD-BAND EMISSION, MOLECULAR CLOUDS, STREAMING, Astrophysics::Galaxy Astrophysics, Astroparticle physics, 010308 nuclear & particles physics, p: relativistic, Institut für Physik und Astronomie, ASTROFÍSICA, gamma ray: VHE, ddc:520, time dependence, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], RAIOS CÓSMICOS
Abstract

著者人数: 382名 (JAXA職員: 井上, 芳幸 : 小山, 志勇 : Lee, Shiu-Hang), Accepted: 2017-04-12, 資料番号: SA1170071000

Published
2017

28. The Arecibo L-band Feed Array Zone of Avoidance (ALFAZOA) Shallow Survey

Author

W. van Driel, T. McIntyre, P. A. Henning, Robert F. Minchin, Stephen E. Schneider, E. Vaez, M. Ramatsoku, Z. Butcher, Emmanuel Momjian, Monica Sanchez-Barrantes, Lister Staveley-Smith, Jessica L. Rosenberg, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, L band, 010308 nuclear & particles physics, FOS: Physical sciences, Zone of Avoidance, Astronomy and Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS
Abstract

The Arecibo L-band Feed Array Zone of Avoidance (ALFAZOA) Shallow Survey is a blind HI survey of the extragalactic sky behind the northern Milky Way conducted with the ALFA receiver on the 305m Arecibo Radio Telescope. ALFAZOA Shallow covered 900 square degrees at full sensitivity from 30{\deg} ${\leq} l {\leq} $75{\deg} and |b|$ {\leq}$ 10{\deg} and an additional 460 square degrees at limited sensitivity at latitudes up to 20{\deg}. It has an rms sensitivity of 5-7 mJy and a velocity resolution of 9 - 20.6 km s$^{-1}$, and detected 403 galaxies out to a recessional velocity of 12,000 km s$^{-1}$, with an angular resolution of 3.4' and a positional accuracy between 0.2' and 1.7'. The survey is complete above an integrated line flux $F_{HI}$ = 2.0 Jy km s$^{-1}$ for half the survey, and above $F_{HI}$ = 2.8 Jy km s$^{-1}$ for the other half. Forty-three percent of the ALFAZOA HI detections have at least one possible optical/NIR counterpart in the literature, and an additional 16% have counterparts that only included previous HI measurements. There are fewer counterparts in regions of high extinction and for galaxies with lower HI mass. Comparing the results of the survey to the predictions of Erdogdu et al. (2006), and using their nomenclature, ALFAZOA confirms the position and extent in the ZOA of the C7, C${\zeta}$, Pegasus, Corona Borealis and Delphinus structures, but not of the Cygnus void. Two new structures are identified, both connected to the C7 overdensity; one extends to 35{\deg}, and the other crosses the ZOA., Comment: 19 pages, 18 figures, accepted for publication in the Astronomical Journal

Published
2019

29. NIBLES – an HI census of stellar mass selected SDSS galaxies

Author

Z. Butcher, W. van Driel, Matthew D. Lehnert, Robert F. Minchin, Stephen E. Schneider, Astronomy Program, University of Massachusetts [Lowell] (UMass Lowell), University of Massachusetts System (UMASS)-University of Massachusetts System (UMASS), Unité Scientifique de la Station de Nançay (USN), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Arecibo Observatory, National Astronomy and Ionosphere Center (NAIC), Cornell University [New York], and Region Centre in France

Subjects
Physics, Stellar mass, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Galaxy, Luminosity, Radio telescope, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, surveys / galaxies: general / galaxies: distances and redshifts / radio lines: galaxies / galaxies: ISM, 010303 astronomy & astrophysics, Line (formation)
Abstract

We obtained Arecibo HI line follow-up observations of 154 of the 2600 galaxies in the Nan\c{c}ay Interstellar Baryons Legacy Extragalactic Survey (NIBLES) sample. These observations are on average four times more sensitive than the original observations at the Nan\c{c}ay Radio Telescope. The main goal of this survey is to characterize the underlying HI properties of the NIBLES galaxies which were undetected or marginally detected at Nan\c{c}ay. Of the Nan\c{c}ay non-detections, 85% were either clearly or marginally detected at Arecibo, while 89% of the Nan\c{c}ay marginal detections were clearly detected. Based on the statistics of the detections relative to g-i color and r-band luminosity (L$_r$) distribution among our Arecibo observations, we anticipate ~60% of our 867 Nan\c{c}ay non-detections and marginal detections could be detected at the sensitivity of our Arecibo observations. Follow-up observations of our low luminosity (L$_r$ < 10$^{8.5}$ L$_{\odot}$) blue sources indicate that they have, on average, more concentrated stellar mass distributions than the Nan\c{c}ay detections in the same luminosity range, suggesting we may be probing galaxies with intrinsically different properties. These follow-up observations enable us to probe HI mass fractions, log($M_{\rm HI}$/$M_{\star}$) 0.5 dex and 1 dex lower, on average, than the NIBLES and ALFALFA surveys respectively., Comment: 22 pages, 13 figures

Published
2016
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30. NIBLES: An H I census of stellar mass selected SDSS galaxies. I. The Nançay H I survey

Author

Stephen E. Schneider, T. Joseph, M. D. Lehnert, A. O. H. Olofsson, P. Kotze, N. Hallet, M. Ramatsoku, R. C. Kraan-Korteweg, L. Chemin, S. L. Blyth, W. van Driel, Robert F. Minchin, Z. Butcher, Astronomy, Unité Scientifique de la Station de Nançay (USN), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Bluestar Silicones, BLUESTAR SILICONES, M2A 2016, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Region Centre in France

Subjects
Physics, radio lines: galaxies, Stellar mass, 010308 nuclear & particles physics, media_common.quotation_subject, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, galaxies: general, Galaxy, Spectral line, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Photometry (optics), Radio telescope, Baryon, galaxies: photometry, Space and Planetary Science, Sky, 0103 physical sciences, Detection rate, galaxies: distances and redshifts, 010303 astronomy & astrophysics, galaxies: ISM, media_common
Abstract

To investigate galaxy properties as a function of their total stellar mass, we obtained 21cm HI line observations at the 100-m class Nan\c{c}ay Radio Telescope of 2839 galaxies from the Sloan Digital Sky Survey (SDSS) in the Local Volume (900, Comment: 71 pages, 14 figures

Published
2016

31. Quantified H i morphology - V. H i discs in the Virgo cluster

Author

W. van Driel, Benne W. Holwerda, Nor Pirzkal, and W. J. G. de Blok

Subjects
Physics, Morphology (linguistics), media_common.quotation_subject, Concentration parameter, Astronomy and Astrophysics, Astrophysics, Asymmetry, Virgo Cluster, Galaxy, Morphological transformation, Space and Planetary Science, Cluster (physics), Truncation (statistics), media_common
Abstract

We explore the quantified morphology of atomic hydrogen (HI) disks in the Virgo cluster. These galaxies display a wealth of phenomena in their Hi morphology, e.g., tails, truncation and warps. These morphological disturbances are related to the ram-pressure stripping and tidal interaction that galaxies undergo in this dense cluster environment. To quantify the morphological transformation of the HI disks, we compute the morphological parameters of CAS, Gini, and M20 and our own GM for 51 galaxies in 48 HI column density maps from the VIVA project. Some morphological phenomena can be identified in this space of relatively low resolution HI data. Truncation of the HI disk can be cleanly identified via the Concentration parameter (C

Published
2011

32. Minor mergers and their impact on the kinematics of galaxy discs

Author

M. D. Lehnert, P. Di Matteo, Y. Qu, W. van Driel, and Chanda J. Jog

Subjects
Physics, General Engineering, Astronomy, Astronomy and Astrophysics, Type-cD galaxy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy merger, Galaxy, Space and Planetary Science, Bulge, Satellite galaxy, Astrophysics::Earth and Planetary Astrophysics, Interacting galaxy, Lenticular galaxy, Astrophysics::Galaxy Astrophysics, Galaxy rotation curve
Abstract

By means of N-body simulations, we have investigated the impact of minor mergers on the angular momentum content and kinematical properties of a disc galaxy. Our simulations cover a range of initial orbital characteristics and the system consists of a massive galaxy with a bulge and a stellar disc merging with a much less massive gasless companion. Our results show that: (1) during the process of merging, the disc of the primary galaxy becomes kinematically hotter and thicker; (2) its specific angular momentum always decreases, independent of the orbit or morphology of the satellite galaxy; (3) the decrease in the rotation velocity of the primary galaxy is accompanied by a change in the anisotropy of the stellar orbits, which becomes increasingly radially dominated as the merger advances; (4) the radial velocity dispersion increases at all radii, but in particular in the outermost regions; (5) at the same time, the transverse velocity decreases throughout the whole disc, except in the inner region, where the constribution of bulge stars leads to an increase of σ t .

Published
2010

33. Can thick disks originate through minor mergers?

Author

Y. Qu, M. D. Lehnert, P. Di Matteo, and W. van Driel

Subjects
Physics, Scale (ratio), Scattering, Minor (linear algebra), General Engineering, Astronomy and Astrophysics, Scale height, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Radius, Galaxy, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Thickening, Astrophysics::Galaxy Astrophysics
Abstract

In this study we use numerical N-body/SPH simulations to investigate the vertical stellar distribution of thick disks formed in minor mergers. These disks have a sech-shape vertical surface density profile which needs two sech functions with different scale heights to fit due to an additional stellar excesses at large heights ( z ≳ 4 − 5 kpc). The scale heights of merger-induced thick disks increase with radius but the details of this thickening are sensitive to orbital configurations and gas fraction of the galaxies. The scale height of the stellar excess is constant with radius and largely independent of the initial conditions. The effects of minor mergers is cumulative in the sense that several minor mergers have the same impact of a single minor merger of the same total mass. Scattering by self-gravitating masses (clumps) in unstable gaseous disks can produce thick disks with constant scale height, however, there is not a stellar excess at large scale heights. Most of these results are found to be in good agreement with observations and thus we conclude that minor mergers remains a viable mechanism for the creation of galactic thick disks.

Published
2010

34. PHYSICAL CONDITIONS IN THE INTERSTELLAR MEDIUM OF INTENSELY STAR-FORMING GALAXIES AT REDSHIFT∼2

Author

W. van Driel, F. Bournaud, Nicole P. H. Nesvadba, L. Chemin, P. Di Matteo, M. D. Lehnert, L. S. Douglas, L. Le Tiran, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Physique des Galaxies et Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)

Subjects
Physics, Star formation, Velocity dispersion, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Redshift, Galaxy, Accretion (astrophysics), Space and Planetary Science, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Surface brightness, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, Line (formation)
Abstract

International audience; We analyze the physical conditions in the interstellar gas of 11 actively star-forming galaxies at z~2, based on integral-field spectroscopy from the ESO-VLT and Hubble Space Telescope/Near Infrared Camera and Multi-Object Spectrometer imaging. We concentrate on the high Halpha surface brightnesses, large line widths, line ratios, and the clumpy nature of these galaxies. We show that photoionization calculations and emission line diagnostics imply gas pressures and densities that are similar to the most intense nearby star-forming regions at z = 0 but over much larger scales (10-20 kpc). A relationship between surface brightness and velocity dispersion can be explained through simple energy injection arguments and a scaling set by nearby galaxies with no free parameters. The high velocity dispersions are a natural consequence of intense star formation thus regions of high velocity dispersion are not evidence for mass concentrations such as bulges or rings. External mechanisms such as cosmological gas accretion generally do not have enough energy to sustain the high velocity dispersions. In some cases, the high pressures and low gas metallicites may make it difficult to robustly distinguish between active galactic nucleus ionization cones and star formation, as we show for BzK-15504 at z = 2.38. We construct a picture where the early stages of galaxy evolution are driven by self-gravity which powers strong turbulence until the velocity dispersion is high. Then massive, dense, gas-rich clumps collapse, triggering star formation with high efficiencies and intensities as observed. At this stage, the intense star formation is likely self-regulated by the mechanical energy output of massive stars.

Published
2009

35. The Arecibo Galaxy Environment Survey - II. A H i view of the Abell cluster 1367 and its outskirts

Author

W. van Driel, Robert F. Minchin, Barbara Catinella, Gregory D. Bothun, Luca Cortese, Stephen E. Schneider, Jonathan Ivor Davies, Karen O'Neil, Giuseppe Gavazzi, Maarten Baes, Jessica L. Rosenberg, A. Boselli, Emmanuel Momjian, R. Taylor, B. S. Koribalski, and Robbie Richard Auld

Subjects
Physics, Baryon, Space and Planetary Science, Cluster (physics), Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Surface brightness, Galaxy, Redshift, Luminosity, Line (formation), Luminosity function (astronomy)
Abstract

We present 21 cm HI line observations of 5x1 square degrees centered on the local Abell cluster 1367 obtained as part of the Arecibo Galaxy Environment Survey. One hundred sources are detected (79 new HI measurements and 50 new redshifts), more than half belonging to the cluster core and its infalling region. Combining the HI data with SDSS optical imaging we show that our HI selected sample follows scaling relations similar to the ones usually observed in optically selected samples. Interestingly all galaxies in our sample appear to have nearly the same baryon fraction independently of their size, surface brightness and luminosity. The most striking difference between HI and optically selected samples resides in their large scale distribution: whereas optical and X-ray observations trace the cluster core very well, in HI there is almost no evidence of the presence of the cluster. Some implications on the determination of the cluster luminosity function and HI distribution for samples selected at different wavelength are also discussed.

Published
2008

36. The Arecibo Galaxy Environment Survey – Potential for finding Dark Galaxies and Results so far

Author

S. Lindner, Rhys Taylor, Stephen E. Schneider, Jonathan Ivor Davies, M. D. Stage, Robbie Richard Auld, Emmanuel Momjian, Erik Muller, W. van Driel, Robert F. Minchin, S. Sabatini, Luca Cortese, Jessica L. Rosenberg, P. A. Henning, Barbara Catinella, and Karen O'Neil

Subjects
Physics, Abell 2744, Space and Planetary Science, Astronomy, Astronomy and Astrophysics, Astrophysics, Dark galaxy, Interacting galaxy, Galaxy merger, Brightest cluster galaxy, Lenticular galaxy, Galaxy, Dwarf galaxy
Abstract

The Arecibo Galaxy Environment Survey is a blind neutral hydrogen survey using the ALFA multibeam receiver at Arecibo Observatory to reach unprecedented sensitivities in a number of selected fields in the local Universe. When completed the survey will cover 200 square degrees out to a distance of at least 270 Mpc. If a population of gas-rich dark galaxies exists, then this survey is in a prime position to uncover that population.So far 20 square degrees have been covered in the regions of Abell 1367, the Virgo Cluster, the NGC 7332/9 galaxy pair and the isolated galaxy NGC 1156. Over 200 sources have been found, including a number that have no obvious optical counterparts. We discuss here the potential of AGES for uncovering more such objects and the characteristics of the dark sources identified to date.

Published
2007

37. Can galaxy growth be sustained through HI-rich minor mergers?

Author

Robert F. Minchin, Matthew D. Lehnert, W. van Driel, Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Unité Scientifique de la Station de Nançay (USN), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université d'Orléans (UO), Arecibo Observatory, National Astronomy and Ionosphere Center (NAIC), Cornell University [New York], Region Centre in France, Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Specific growth, Stellar mass, Minor (linear algebra), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Accretion rate, galaxies: high-redshift, 0103 physical sciences, galaxies: formation, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, galaxies: kinematics and dynamics, Astrophysics::Galaxy Astrophysics, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Unit mass, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution
Abstract

Local galaxies with specific star-formation rates (star-formation rate per unit mass; sSFR~0.2-10/Gyr) as high as distant galaxies (z~1-3), are very rich in HI. Those with low stellar masses, log M_star (M_sun)=8-9, for example, have M_HI/M_star~5-30. Using continuity arguments of Peng et al. (2014), whereby the specific merger rate is hypothesized to be proportional to the specific star-formation rate, and HI gas mass measurements for local galaxies with high sSFR, we estimate that moderate mass galaxies, log M_star (M_sun)=9-10.5, can acquire sufficient gas through minor mergers (stellar mass ratios ~4-100) to sustain their star formation rates at z~2. The relative fraction of the gas accreted through minor mergers declines with increasing stellar mass and for the most massive galaxies considered, log M_star (M_sun)=10.5-11, this accretion rate is insufficient to sustain their star formation. We checked our minor merger hypothesis at z=0 using the same methodology but now with relations for local normal galaxies and find that minor mergers cannot account for their specific growth rates, in agreement with observations of HI-rich satellites around nearby spirals. We discuss a number of attractive features, like a natural down-sizing effect, in using minor mergers with extended HI disks to support star formation at high redshift. The answer to the question posed by the title, "Can galaxy growth be sustained through \HI-rich minor mergers?", is maybe, but only for relatively low mass galaxies and at high redshift., 6 pages, 3 figures; in final acceptance by A&A

Published
2015

38. On the cosmic evolution of the specific star formation rate

Author

Misha Haywood, L. Le Tiran, Matthew D. Lehnert, P. Di Matteo, W. van Driel, Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Observatoire de Paris - Site de Paris (OP), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), and Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, Angular momentum, Stellar mass, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Star formation, Hydrostatic pressure, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Stars, Space and Planetary Science, galaxies: high-redshift, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, Astrophysics::Galaxy Astrophysics, galaxies: kinematics and dynamics, galaxies: ISM, Line (formation)
Abstract

The apparent correlation between the specific star formation rate (sSFR) and total stellar mass (M_star) of galaxies is a fundamental relationship indicating how they formed their stellar populations. To attempt to understand this relation, we hypothesize that the relation and its evolution is regulated by the increase in the stellar and gas mass surface density in galaxies with redshift, which is itself governed by the angular momentum of the accreted gas, the amount of available gas, and by self-regulation of star formation. With our model, we can reproduce the specific SFR-M_star relations at z~1-2 by assuming gas fractions and gas mass surface densities similar to those observed for z=1-2 galaxies. We further argue that it is the increasing angular momentum with cosmic time that causes a decrease in the surface density of accreted gas. The gas mass surface densities in galaxies are controlled by the centrifugal support (i.e., angular momentum), and the sSFR is predicted to increase as, sSFR(z)=(1+z)^3/t_H0, as observed (where t_H0 is the Hubble time and no free parameters are necessary). At z>~2, we argue that star formation is self-regulated by high pressures generated by the intense star formation itself. The star formation intensity must be high enough to either balance the hydrostatic pressure (a rather extreme assumption) or to generate high turbulent pressure in the molecular medium which maintains galaxies near the line of instability (i.e. Toomre Q~1). The most important factor is the increase in stellar and gas mass surface density with redshift, which allows distant galaxies to maintain high levels of sSFR. Without a strong feedback from massive stars, such galaxies would likely reach very high sSFR levels, have high star formation efficiencies, and because strong feedback drives outflows, ultimately have an excess of stellar baryons (abridged)., A&A accepted, 13 pages

Published
2015

39. NenuFAR: Instrument description and science case

Author

Sylvain Azarian, A. Bosma, Chiara Ferrari, A. Petiteau, Loïc Denis, M. Pandey-Pommier, Luitje Koopmans, Remy Boyer, M. Arnaud, C. Taffoureau, Jean-Louis Pinçon, David Mary, Giulia Macario, M. N. El Korso, A. A. Konovalenko, Jean-Jacques Maintoux, W. van Driel, Marcellin Atemkeng, Didier Charrier, Ismaël Cognard, Peter L. Tokarsky, B. Guiderdoni, Benoît Revenu, A. Loh, Annalisa Bonafede, J. Vaubaillon, A. Ferrari, S. Daiboo, S. Masson, M. Serylak, Edith Falgarone, Francoise Combes, F. Levrier, Gilles Theureau, P. Salome, Mykhaylo Panchenko, Arwa Dabbech, M.-A. Miville-Deschenes, B. Semelin, M. Was, Jason W. T. Hessels, J.-M. Griebmeier, Frederic Boone, Carine Briand, Rodolphe Weber, E. Gerard, C. Fevotte, Frederic Rible, S. D. Vergani, V. V. Zakharenko, Cedric Dumez-Viou, V. I. Kondratiev, Julien N. Girard, E. Chassande-Mottin, T. Lanz, L. Lamy, Oleg Smirnov, M. Fullekrug, O. M. Ulyanov, Franco Vazza, Benjamin Stappers, C. Tasse, P. Zarka, M. Tagger, C. Courte, M. Branchesi, Lucas Guillemot, Matt Lehnert, Baptiste Cecconi, Steve Torchinsky, I. Falkovych, D. Oberoi, Richard Dallier, A. Coffre, M. Barsuglia, I. Y. Vasylieva, Stephane Corbel, Katia Ferrière, Helmut O. Rucker, L. Martin, A. Fialkov, S. Celestin, Cédric Richard, Pascal Larzabal, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire des signaux et systèmes (L2S), Université Paris-Sud - Paris 11 (UP11)-CentraleSupélec-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire de physique subatomique et des technologies associées (SUBATECH), Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-IMT Atlantique (IMT Atlantique), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT), Collège de France - Chaire Galaxies et cosmologie, Collège de France (CdF (institution)), Laboratoire d'Etudes et Recherche en Mathématiques Appliquées (LERMA), Ecole Mohammadia d'Ingénieurs (EMI), Laboratoire Energétique Mécanique Electromagnétisme (LEME), Université Paris Nanterre (UPN), Systèmes et Applications des Technologies de l'Information et de l'Energie (SATIE), École normale supérieure - Cachan (ENS Cachan)-Université Paris-Sud - Paris 11 (UP11)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-École normale supérieure - Rennes (ENS Rennes)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Conservatoire National des Arts et Métiers [CNAM] (CNAM), HESAM Université - Communauté d'universités et d'établissements Hautes écoles Sorbonne Arts et métiers université (HESAM)-HESAM Université - Communauté d'universités et d'établissements Hautes écoles Sorbonne Arts et métiers université (HESAM)-Centre National de la Recherche Scientifique (CNRS), Laboratoire SUBATECH Nantes (SUBATECH), Mines Nantes (Mines Nantes)-Université de Nantes (UN)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Unité Scientifique de la Station de Nançay (USN), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire Pluridisciplinaire de Recherche en Ingénierie des Systèmes, Mécanique et Energétique (PRISME), Université d'Orléans (UO)-Ecole Nationale Supérieure d'Ingénieurs de Bourges (ENSI Bourges), NenuFAR, ANR-14-CE23-0004,MAGELLAN,Méthodes d'apprentissage pour les très grands réseaux d'antennes en radioastronomie(2014), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université de Nantes (UN)-Université de Nantes (UN)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), Chaire Galaxies et cosmologie, Université Paris-Seine-Université Paris-Seine-Conservatoire National des Arts et Métiers [CNAM] (CNAM)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Nantes (UN)-Mines Nantes (Mines Nantes), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), Ecole Nationale Supérieure d'Ingénieurs de Bourges (ENSI Bourges)-Université d'Orléans (UO), École normale supérieure - Rennes (ENS Rennes)-Université Paris-Sud - Paris 11 (UP11)-Conservatoire National des Arts et Métiers [CNAM] (CNAM)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Université de Cergy Pontoise (UCP), and Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Cachan (ENS Cachan)-Université Gustave Eiffel (UNIV GUSTAVE EIFFEL)

Subjects
Antenna design, 02 engineering and technology, radio astronomy, radio telescope, antenna array, antenna effective area, 01 natural sciences, Antenna array, Radio telescope, [SPI]Engineering Sciences [physics], 0103 physical sciences, 0202 electrical engineering, electronic engineering, information engineering, Radiotelescope, Low frequency radioastronomy, Radio astronomy, 010303 astronomy & astrophysics, Antenna Arrays, Physics, Scope (project management), business.industry, NenuFAR, 020206 networking & telecommunications, LOFAR, Pathfinder, Antenna (radio), Telecommunications, business, antennas, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; NenuFAR is both a giant extension of the LOFAR and a large standalone instrument in the low-frequency range (10-85 MHz). It was designed in Nançay with national and international collaboration. Antenna radiators were modeled on the LWA antenna design whereas preamplifiers were designed in France. Antennas will be distributed in 96 mini-arrays of 19 dual-polarized elements, densely covering a disk of 400 m in diameter. A few mini-arrays are expected to lie at distances of 2-3 km. A silent control-command system was designed, and the computer dialog with LOFAR defined. Receivers will include the LOFAR backend, a local beamformer and a local correlator. NenuFAR is in construction in Nançay and it was recently granted by the SKA office the official label of SKA pathfinder. Its exploitation will expand the scope of LOFAR scientific studies as well as permit new studies, preparing for SKA science. The NenuFAR concept has many points in common with GURT (the Giant Ukrainian Radio Telescope), with which it shares some technical studies, an its exploitation will benefit from a coordination with UTR-2. We describe the instrument, technical developments and science case.

Published
2015

40. Subarcsecond international LOFAR radio images of the M82 nucleus at 118 MHz and 154 MHz

Author

R.-J. Dettmar, B. Adebahr, Marcus Brüggen, Rainer Beck, Ivan Marti-Vidal, Tobia Carozzi, Glenn J. White, Eskil Varenius, Matt J. Jarvis, J. Moldon, Gianfranco Brunetti, Cathy Horellou, Philip Best, Neal Jackson, W. van Driel, M. C. Toribio, Marijke Haverkorn, Robert Beswick, Olaf Wucknitz, Miguel A. Pérez-Torres, Susanne Aalto, George Heald, Leah K. Morabito, Krzysztof T. Chyzy, Adam T. Deller, George K. Miley, John Conway, H. J. A. Röttgering, Onsala Space Observatory, Dept. of Radio and Space Science, Chalmers University of Technology, Chalmers University of Technology [Göteborg], Netherlands Institute for Radio Astronomy (ASTRON), Argelander-Institut für Astronomie (AlfA), Rheinische Friedrich-Wilhelms-Universität Bonn, Swedish Institute of Space Physics [Uppsala] (IRF), Departament d'Astronomia i Meteorologia [Barcelona], Universitat de Barcelona (UB), University of Edinburgh, Astronomisches Institut der Ruhr-Universität Bochum, Ruhr-Universität Bochum [Bochum], Observatoire de Paris - Site de Paris (OP), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Jacobs University [Bremen], Radboud university [Nijmegen], Department of Earth and Space Sciences [Göteborg], Centre d'études européennes et de politique comparée (CEE), Centre National de la Recherche Scientifique (CNRS)-Sciences Po (Sciences Po), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Physics Department, Queen Mary and Westfield College, Queen Mary University of London (QMUL), Institut de Ciènces del Cosmos (ICC), Universitat de Barcelona (UB)-Universitat de Barcelona (UB), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), and Astronomy

Subjects
Brightness, Astronomy, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Starburst region, galaxies: starburst, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, law.invention, Telescope, galaxies: individual: M82, law, Very-long-baseline interferometry, Astronomy, Astrophysics and Cosmology, Image resolution, Astrophysics::Galaxy Astrophysics, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Star formation, starburst [galaxies], high angular resolution [techniques], techniques: high angular resolution, Astronomy and Astrophysics, LOFAR, Astrophysics - Astrophysics of Galaxies, Galaxy, supernovae: individual: 2008iz, interferometric [techniques], Space and Planetary Science, techniques: interferometric, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), galaxies: star formation, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, individual: M82 [galaxies], star formation [galaxies], individual: 2008iz [supernovae]
Abstract

The nuclear starburst in the nearby galaxy M82 provides an excellent laboratory for understanding the physics of star formation. This galaxy has been extensively observed in the past, revealing tens of radio-bright compact objects embedded in a diffuse free-free absorbing medium. Our understanding of the structure and physics of this medium in M82 can be greatly improved by high-resolution images at low frequencies where the effects of free-free absorption are most prominent. The aims of this study are, firstly, to demonstrate imaging using international baselines of the Low Frequency Array (LOFAR), and secondly, to constrain low-frequency spectra of compact and diffuse emission in the central starburst region of M82 via high-resolution radio imaging at low frequencies. The international LOFAR telescope was used to observe M82 at 110-126MHz and 146-162MHz. Images were obtained using standard techniques from very long baseline interferometry. images were obtained at each frequency range: one only using international baselines, and one only using the longest Dutch (remote) baselines. The 154MHz image obtained using international baselines is a new imaging record in terms of combined image resolution (0.3$"$) and sensitivity ($\sigma$=0.15mJy/beam) at low frequencies ($, Comment: 15 pages, 7 figures

Published
2015

41. Upflow Reactors for Riparian Zone Denitrification

Author

Peter W. van Driel, L. Craig Merkley, and William D. Robertson

Subjects
Environmental Engineering, Denitrification, Nitrogen, Water flow, Analytical chemistry, chemistry.chemical_element, Management, Monitoring, Policy and Law, Water Purification, Bioreactors, Rivers, Hydraulic conductivity, Water Supply, Water Movements, Waste Management and Disposal, Water Science and Technology, Riparian zone, Hydrology, geography, Nitrates, geography.geographical_feature_category, Chemistry, Agriculture, Models, Theoretical, Wood, Pollution, Aerosol, Biodegradation, Environmental, Permeable reactive barrier, Surface water, Water Pollutants, Chemical
Abstract

We used permeable reactive subsurface barriers consisting of a C source (wood particles), with very high hydraulic conductivities ( approximately 0.1-1 cm s(-1)), to provide high rates of riparian zone NO3-N removal at two field sites in an agricultural area of southwestern Ontario. At one site, a 0.73-m3 reactor containing fine wood particles was monitored for a 20-mo period and achieved a 33% reduction in mean influent NO3-N concentration of 11.5 mg L(-1) and a mean removal rate of 4.5 mg L(-1) d(-1) (0.7 g m(-2) d(-1)). At the second site, four smaller reactors (0.21 m3 each), two containing fine wood particles and two containing coarse wood particles, were monitored for a 4-mo period and were successful in attenuating mean influent NO3-N concentrations of 23.7 to 35.1 mg L(-1) by 41 to 63%. Mean reaction rates for the two coarse-particle reactors (3.2 and 7.8 mg L(-1) d(-1), or 1.5 and 3.4 g m(-2) d(-1)) were not significantly different (p > 0.2) than the rates observed in the two fine-particle reactors (5.0 and 9.9 mg L(-1) d(-1), or 1.8-3.5 g m(-2) d(-1)). A two-dimensional ground water flow model is used to illustrate how permeable reactive barriers such as these can be used to redirect ground water flow within riparian zones, potentially augmenting NO3- removal in this environment.

Published
2006

42. NGC 4254: a spiral galaxy entering the Virgo cluster

Author

W. Huchtmeier, W. van Driel, and B. Vollmer

Subjects
Physics, Spiral galaxy, Orbital plane, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Virgo Cluster, Spectral line, Galaxy, Ram pressure, Space and Planetary Science, Astrophysics::Galaxy Astrophysics, Spiral, Line (formation)
Abstract

Deep Effelsberg HI spectra of the one-armed, bright Virgo cluster spiral galaxy NGC 4254 are presented.Five different positions were observed in the 21 cm HI line with the Effelsberg 100-m telescope: one in the center and 4 located one HPBW to the NE, NW, SW, and SE, respectively, from the galaxy center. The spectra are compared to existing deep VLA observations, and the single dish and interferometric HI data are used to constrain a dynamical model which includes the effects of ram pressure. The peculiar, one-armed spiral pattern of NGC 4254 and its distorted and kinematically perturbed atomic gas distribution can be explained by a close and rapid encounter ~280 Myr ago with another massive Virgo galaxy, followed by ram pressure stripping that is still ongoing. The stripping occurs almost face-on, since the angle between the disk and the orbital plane is 70 degrees. The galaxy with which NGC 4254 had its encounter is tentatively identified as the lenticular NGC 4262., 15 pages, 13 figure. Accepted for publication in A&A

Published
2005

43. The dwarf low surface brightness galaxy population of the Virgo Cluster - II. Colours and H i line observations

Author

S. Sabatini, J. Davies, W. van Driel, M. Baes, S. Roberts, R. Smith, S. Linder, and K. O'Neil

Subjects
Physics, education.field_of_study, Star formation, Population, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Virgo Cluster, Galaxy, Ram pressure, Supernova, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Surface brightness, education, Astrophysics::Galaxy Astrophysics, Dwarf galaxy
Abstract

In order to investigate the nature of dwarf Low Surface Brightness (LSB) galaxies we have undertaken a deep B and I band CCD survey of a 14 sq degree strip in the Virgo Cluster and applied a Fourier convolution technique to explore its dwarf galaxy population down to a central surface brightness of � 26 B mag/ arcsec 2 and a total absolute B mag of � -10. In this paper we carry out an analysis of their morphology, (B-I) colours and atomic hydrogen content. We compare these properties with those of dwarf galaxies in other environments to try and assess how the cluster environment has influenced their evolution. Field dwarfs are generally of a more irregular morphology, are bluer and contain relatively more gas. We assess the importance that various physical processes have on the evolution of cluster dwarf galaxies (ram pressure stripping, tidal interactions, supernova driven gas loss). We suggest that enhanced star formation triggered by tidal interactions is the major reason for the very different general properties of cluster dwarfs: they have undergone accelerated evolution.

Published
2005

44. A method for determining radio continuum spectra and its application to large surveys

Author

E. Davoust, W. van Driel, Françoise Genova, Bernd Vollmer, François Ochsenbein, Pascal Dubois, Laboratoire Gemini (LG), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Radioastronomie (MPIfR), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Physique des Galaxies et Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, Spectral index, Mean squared error, Astrophysics (astro-ph), Continuum (design consultancy), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Spectral line, Variable (computer science), [SDU]Sciences of the Universe [physics], Space and Planetary Science, Code (cryptography), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Remote sensing
Abstract

A new tool to extract cross-identifications and radio continuum spectra from radio catalogues contained in the VIZIER database of the CDS is presented. The code can handle radio surveys at different frequencies with different resolutions. It has been applied to 22 survey catalogues at 11 different frequencies containing a total of 3.5 million sources, which resulted in over 700000 independent radio cross-identifications and ~67000 independent radio spectra with more than two frequency points. A validation of the code has been performed using independent radio cross-correlations from the literature. The mean error of the determined spectral index is +-0.3. The code produces an output of variable format that can easily be adapted to the purpose of the user., Comment: 11 pages, 11 figures. Accepted for publication in A&A

Published
2005

45. Galaxy transmutations: The double ringed galaxy ESO 474-G26

Author

Frederic Bournaud, Francoise Combes, M. Faúndez-Abans, M. de Oliveira-Abans, V. P. Reshetnikov, W. van Driel, Stephen E. Schneider, Astronomical Institute of St. Petersburg State University, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Galaxies et cosmologie, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Laboratório Nacional de Astrofísica, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Physique des Galaxies et Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), and University of Massachusetts, Astronomy Program

Subjects
Physics, Effective radius, Spiral galaxy, Astrophysics (astro-ph), FOS: Physical sciences, Equatorial ring, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy merger, Polar-ring galaxy, Galaxy, Space and Planetary Science, Elliptical galaxy, Surface brightness, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics
Abstract

Surface photometry and a 21cm HI line spectrum of the giant double-ringed galaxy ESO 474-G26 are presented. The morphology of this system is unique among the 30,000 galaxies with >B15. Two almost orthogonal optical rings with diameters of 60 and 40 kpc surround the central body (assuming H0=70 km/s/Mpc). The outer one is an equatorial ring, while the inner ring lies in a nearly polar plane. The rings have blue optical colors typical of late-type spirals. Both appear to be rotating around the central galaxy, so that this system can be considered as a kinematically confirmed polar ring galaxy. Its observational characteristics are typical of galaxy merger remnants. Although the central object has a surface brightness distribution typical of elliptical galaxies, it has a higher surface brightness for its effective radius than ordinary ellipticals. Possible origins of this galaxy are discussed and numerical simulations are presented that illustrate the formation of the two rings in the merging process of two spiral galaxies, in which the observed appearance of ESO 474-G26 appears to be a transient stage., Accepted for publication in A&A

Published
2005

46. A multibeam H i survey of the Virgo cluster - two isolated H i clouds?

Author

R. H. Lang, S.M. Roberts, Virginia A. Kilborn, S. Linder, S. Sabatini, M. J. Disney, P. J. Boyce, Randall B. Smith, Jonathan Ivor Davies, Maarten Baes, W. van Driel, Robert F. Minchin, Rh. Evans, and W. J. G. de Blok

Subjects
Physics, Field galaxy, Astrophysics (astro-ph), HIPASS, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Virgo Cluster, Galaxy, Delta-v (physics), Space and Planetary Science, Sensitivity (control systems), Low Mass, Luminosity function (astronomy)
Abstract

We have carried out a fully sampled large area ($4^{\circ} \times 8^{\circ}$) 21cm \HI line survey of part of the Virgo cluster using the Jodrell Bank multi-beam instrument. The survey has a sensitivity some 3 times better than the standard HIJASS and HIPASS surveys. We detect 31 galaxies, 27 of which are well known cluster members. The four new detections have been confirmed in the HIPASS data and by follow up Jodrell Bank pointed observations. One object lies behind M86, but the other 3 have no obvious optical counter parts upon inspection of the digital sky survey fields. These 3 objects were mapped at Arecibo with a smaller \am{3}{6} HPBW and a 4 times better sensitivity than the Jodrell Bank data, which allow an improved determination of the dimensions and location of two of the objects, but surprisingly failed to detect the third. The two objects are resolved by the Arecibo beam giving them a size far larger than any optical images in the nearby field. To our mass limit of $5 \times 10^{7}$ $\frac{\Delta v}{50 km s^{-1}}$ $M_{\odot}$ and column density limit of $3 \times 10^{18}$ $\frac{\Delta v}{50 km s^{-1}}$ atoms cm$^{-2}$ these new detections represent only about 2% of the cluster atomic hydrogen mass. Our observations indicate that the \HI mass function of the cluster turns down at the low mass end making it very different to the field galaxy \HI mass function. This is quite different to the Virgo cluster optical luminosity function which is much steeper than that in the general field. Many of the sample galaxies are relatively gas poor compared to \HI selected samples of field galaxies, confirming the 'anaemic spirals' view of Virgo cluster late type galaxies., Comment: Accepted for publication in MNRAS

Published
2004

47. The GALEX Ultraviolet Virgo Cluster Survey (GUViCS). I: The UV luminosity function of the central 12 sq.deg

Author

Laura Ferrarese, Emmanuel Momjian, Leslie K. Hunt, Eric Emsellem, J. I. Davies, Catherine Vlahakis, José M. Solanes, Noah Brosch, Matthew Smith, Jacopo Fritz, Andrés Jordán, Kelley M. Hess, James E. Taylor, W. van Driel, I. De Looze, Marco Grossi, Samuel Boissier, Patrick R. Durrell, Maarten Baes, Alessandro Boselli, S. di Serego Alighieri, Thomas Erben, Simona Mei, Sebastien Heinis, Pierre-Alain Duc, Thomas M. Hughes, Emmanuel M. Xilouris, O. Spector, Brian R. Kent, D. A. Garcia-Appadoo, Emmanouil Papastergis, Giuseppe Gavazzi, C. Balkowski, Bernd Vollmer, Kristine Spekkens, O. Ilbert, Laura Magrini, Lauren A. MacArthur, Riccardo Giovanelli, O. Cucciati, Suzanne C. Madden, Ariane Lançon, Marcel Clemens, C. Valotto, Vassilis Charmandaris, Luca Cortese, Marc Huertas-Company, Martha P. Haynes, Joris Verstappen, Scott Chapman, Aliakbar Dariush, Diego G. Lambas, Ronald P. Olowin, Astronomy, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), A. Boselli, S. Boissier, S. Heini, L. Cortese, O. Ilbert, T. Hughe, O. Cucciati, J. Davie, L. Ferrarese, R. Giovanelli, M. P. Hayne, M. Bae, C. Balkowski, N. Brosch, S. C. Chapman, V. Charmandari, M. S. Clemen, A. Dariush, I. De Looze, S. di Serego Alighieri, P.-A. Duc, P. R. Durrell, E. Emsellem, T. Erben, J. Fritz, D. A. Garcia-Appadoo, G. Gavazzi, M. Grossi, A. Jordán, K. M. He, M. Huertas-Company, L. K. Hunt, B. R. Kent, D. G. Lamba, A. Lançon, L. A. MacArthur, S. C. Madden, L. magrini, S. Mei, E. Momjian, R. P. Olowin, E. Papastergi, M. W. L. Smith, J. M. Solane, O. Spector, K. Spekken, J. E. Taylor, C. Valotto, W. van Driel, J. Verstappen, C. Vlahaki, B. Vollmer, and E. M. Xilouris

Subjects
HI SOURCE CATALOG, Cosmology and Nongalactic Astrophysics (astro-ph.CO), COMA CLUSTER, FAST ALPHA SURVEY, DATA RELEASE, NEARBY CLUSTERS, FOS: Physical sciences, DWARF ELLIPTIC GALAXIES, Astrophysics, medicine.disease_cause, 01 natural sciences, Luminosity, STAR-FORMATION, 0103 physical sciences, Galaxy formation and evolution, medicine, Cluster (physics), fundamental parameters [galaxies], EARLY-TYPE GALAXIES, 010303 astronomy & astrophysics, galaxies: fundamental parameter, evolution [galaxies], Luminosity function (astronomy), luminosity function [galaxies], Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, galaxies: fundamental parameters, clusters: individual: Virgo [galaxies], BAND SURFACE PHOTOMETRY, Virgo Cluster, Galaxy, galaxies: luminosity function, Physics and Astronomy, Space and Planetary Science, mass function, galaxies: luminosity function, mass function, galaxies: clusters: individual: Virgo, ultraviolet: galaxies, astro-ph.CO, ultraviolet: galaxie, DIGITAL SKY SURVEY, galaxies [ultraviolet], galaxies: evolution, Ultraviolet, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS) is a complete blind survey of the Virgo cluster covering about 40 sq. deg. in the far UV (FUV, lambda_eff=1539A, Delta-lambda=442A) and about 120 sq. deg. in the near UV (NUV, lambda_eff=2316A, Delta-lambda=1060A). The goal of the survey is to study the ultraviolet (UV) properties of galaxies in a rich cluster environment, spanning a wide luminosity range from giants to dwarfs, and regardless of prior knowledge of their star formation activity. The UV data will be combined with those in other bands (optical: NGVS; far-infrared - submm: HeViCS; HI: ALFALFA) and with our multizone chemo-spectrophotometric models of galaxy evolution to make a complete and exhaustive study of the effects of the environment on the evolution of galaxies in high density regions. We present here the scientific objectives of the survey, describing the observing strategy and briefly discussing different data reduction techniques. Using UV data already in-hand for the central 12 sq. deg. we determine the FUV and NUV luminosity functions of the Virgo cluster core for all cluster members and separately for early- and late-type galaxies and compare it to the one obtained in the field and other nearby clusters (Coma, A1367). This analysis shows that the FUV and NUV luminosity functions of the core of the Virgo clusters are flatter (alpha about -1.1) than those determined in Coma and A1367. We discuss the possible origin of this difference, 18 pages, 14 figures, accepted in A&A, high resolution version of figure 1 and 2 and other information available at http://galex.oamp.fr/guvics/observations.html

Published
2011

48. Chemical and spectrophotometric evolution of low surface brightness galaxies

Author

D. Monnier Ragaigne, C. Balkowski, Nikos Prantzos, Karen O'Neil, Samuel Boissier, and W. van Driel

Subjects
Physics, Brightness, Angular momentum, Star formation, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, High surface, Space and Planetary Science, Homogeneous, Computer Science::Multimedia, Astrophysics::Solar and Stellar Astrophysics, Surface brightness, Astrophysics::Galaxy Astrophysics
Abstract

Based on the results of recent surveys, we have constructed a relatively homogeneous set of observational data concerning the chemical and photometric properties of Low Surface Brightness galaxies (LSBs). We have compared the properties of this data set with the predictions of models of the chemical and spectrophotometric evolution of LSBs. The basic idea behind the models, i.e. that LSBs are similar to 'classical' High Surface Brightness spirals except for a larger angular momentum, is found to be consistent with the results of their comparison with these data. However, some observed properties of the LSBs (e.g. their colours, and specifically the existence of red LSBs) as well as the large scatter in these properties, cannot be reproduced by the simplest models with smoothly evolving star formation rates over time. We argue that the addition of bursts and/or truncations in the star formation rate histories can alleviate that discrepancy., Comment: Accepted in MNRAS. 14 pages. 13 figures

Published
2003

49. Non-confirmation of reported $\ion{H}{I}$ clouds without optical counterparts in the Hercules cluster

Author

P. Papaderos, C. Balkowski, José M. Vílchez, V. Cayatte, Trinh X. Thuan, John M. Dickey, W. van Driel, H. Hernández, Karen O'Neil, Pierre-Alain Duc, Jorge Iglesias-Páramo, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Physique des Galaxies et Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Arecibo Observatory, Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Department of Astronomy, University of Minnesota, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Sternwarte Weinheim, Instituto de Astrofisica de Andalucia, CSIC (IAA), and Astronomy Department, University of Virginia, Charlottesville

Subjects
Physics, Gregorian telescope, Galactic astronomy, Continuum (measurement), 010308 nuclear & particles physics, media_common.quotation_subject, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, general, clusters, individual, Hercules cluster, galaxies, ISM, radio lines, 01 natural sciences, law.invention, Space and Planetary Science, law, Sky, 0103 physical sciences, Surface brightness, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, media_common
Abstract

21 cm HI line observations were made with the Arecibo Gregorian telescope of 9 HI clouds in the Hercules Cluster which were reported as tenative detections in a VLA HI study of the cluster (Dickey 1997) and for which our deep CCD imaging failed to find any optical counterparts. No sensitive observations could be made of one of these (sw-174) due to the presence of a close-by strong continuum source. The other 8 tentative HI detections were not reconfirmed by the Arecibo HI measurements. The CCD images did reveal faint, low surface brightness counterparts near the centres of two other VLA HI sources invisible on the Palomar Sky Survey, sw-103 and sw-194., Comment: 7 pages, accepted for Astronomy and Astrophysics on 8 Nov. 2002; new references added on 23 Dec. 2002

Published
2003

50. [Untitled]

Author

C. Balkowski, S. Boissier, D. Monnier Ragaigne, Nikos Prantzos, and W. van Driel

Subjects
Physics, Space and Planetary Science, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Surface brightness, Disc galaxy, Astrophysics::Galaxy Astrophysics, Galaxy
Abstract

We show that simple models of the chemical and spectrophotometric evolution of galaxies can be used to explore the properties of present-day galaxies and especially the causes of the observed variety among disc galaxies. We focus on the link between ``classical'' spirals and Low Surface Brightness galaxies.

Published
2003

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