189 results on '"Smolcic, V."'
Search Results
152. ERRATUM: “PHOTOMETRIC PROPERTIES OF Lyα EMITTERS AT z ≈ 4.86 IN THE COSMOS 2 SQUARE DEGREE FIELD” (2009, ApJ, 696, 546)
- Author
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Shioya, Y., primary, Taniguchi, Y., additional, Sasaki, S. S., additional, Nagao, T., additional, Murayama, T., additional, Saito, T., additional, Ideue, Y., additional, Nakajima, A., additional, Matsuoka, K., additional, Trump, J., additional, Scoville, N. Z., additional, Sanders, D. B., additional, Mobasher, B., additional, Aussel, H., additional, Capak, P., additional, Kartaltepe, J., additional, Koekemoer, A., additional, Carilli, C., additional, Ellis, R. S., additional, Garilli, B., additional, Giavalisco, M., additional, Kitzbichler, M. G., additional, Impey, C., additional, LeFevre, O., additional, Schinnerer, E., additional, and Smolcic, V., additional
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- 2009
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153. PHOTOMETRIC PROPERTIES OF Lyα EMITTERS ATz≈ 4.86 IN THE COSMOS 2 SQUARE DEGREE FIELD
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Shioya, Y., primary, Taniguchi, Y., additional, Sasaki, S. S., additional, Nagao, T., additional, Murayama, T., additional, Saito, T., additional, Ideue, Y., additional, Nakajima, A., additional, Matsuoka, K., additional, Trump, J., additional, Scoville, N. Z., additional, Sanders, D. B., additional, Mobasher, B., additional, Aussel, H., additional, Capak, P., additional, Kartaltepe, J., additional, Koekemoer, A., additional, Carilli, C., additional, Ellis, R. S., additional, Garilli, B., additional, Giavalisco, M., additional, Kitzbichler, M. G., additional, Impey, C., additional, LeFevre, O., additional, Schinnerer, E., additional, and Smolcic, V., additional
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- 2009
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154. CHASING HIGHLY OBSCURED QSOs IN THE COSMOS FIELD
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Fiore, F., primary, Puccetti, S., additional, Brusa, M., additional, Salvato, M., additional, Zamorani, G., additional, Aldcroft, T., additional, Aussel, H., additional, Brunner, H., additional, Capak, P., additional, Cappelluti, N., additional, Civano, F., additional, Comastri, A., additional, Elvis, M., additional, Feruglio, C., additional, Finoguenov, A., additional, Fruscione, A., additional, Gilli, R., additional, Hasinger, G., additional, Koekemoer, A., additional, Kartaltepe, J., additional, Ilbert, O., additional, Impey, C., additional, Le Floc'h, E., additional, Lilly, S., additional, Mainieri, V., additional, Martinez-Sansigre, A., additional, McCracken, H. J., additional, Menci, N., additional, Merloni, A., additional, Miyaji, T., additional, Sanders, D. B., additional, Sargent, M., additional, Schinnerer, E., additional, Scoville, N., additional, Silverman, J., additional, Smolcic, V., additional, Steffen, A., additional, Santini, P., additional, Taniguchi, Y., additional, Thompson, D., additional, Trump, J. R., additional, Vignali, C., additional, Urry, M., additional, and Yan, L., additional
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- 2009
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155. Properties of the molecular gas in a starbursting QSO at z = 1.83 in the COSMOS field
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Aravena, M., primary, Bertoldi, F., additional, Schinnerer, E., additional, Weiss, A., additional, Jahnke, K., additional, Carilli, C. L., additional, Frayer, D., additional, Henkel, C., additional, Brusa, M., additional, Menten, K. M., additional, Salvato, M., additional, and Smolcic, V., additional
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- 2008
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156. COSBO: The MAMBO 1.2 Millimeter Imaging Survey of the COSMOS Field
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Bertoldi, F., primary, Carilli, C., additional, Aravena, M., additional, Schinnerer, E., additional, Voss, H., additional, Smolcic, V., additional, Jahnke, K., additional, Scoville, N., additional, Blain, A., additional, Menten, K. M., additional, Lutz, D., additional, Brusa, M., additional, Taniguchi, Y., additional, Capak, P., additional, Mobasher, B., additional, Lilly, S., additional, Thompson, D., additional, Aussel, H., additional, Kreysa, E., additional, Hasinger, G., additional, Aguirre, J., additional, Schlaerth, J., additional, and Koekemoer, A., additional
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- 2007
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157. The XXL survey: first results and future
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Pierre, M., Adami, C., Birkinshaw, M., Chiappetti, L., Ettori, S., Evrard, A., Faccioli, L., Gastaldello, F., Giles, P., Horellou, C., Iovino, A., Koulouridis, E., Lidman, C., Brun, A. Le, Maughan, B., Maurogordato, S., McCarthy, I., Miyazaki, S., Pacaud, F., Paltani, S., Plionis, M., Reiprich, T., Sadibekova, T., Smolcic, V., Snowden, S., Surdej, J., Tsirou, M., Vignali, C., Willis, J., Alis, S., Altieri, B., Baran, N., Benoist, C., Bongiorno, A., Bremer, M., Butler, A., Cappi, A., Caretta, C., Ciliegi, P., Clerc, N., Corasaniti, P. S., Coupon, J., Delhaize, J., Delvecchio, I., Democles, J., Desai, Sh., Devriendt, J., Dubois, Y., Eckert, D., Elyiv, A., Farahi, A., Ferrari, C., Fotopoulou, S., Forman, W., Georgantopoulos, I., Guglielmo, V., Huynh, M., Jerlin, N., Jones, Ch., Lavoie, S., Fevre, J. -P. Le, Lieu, M., Kilbinger, M., Marulli, F., Mantz, A., McGee, S., Melin, J. -B., Melnyk, O., Moscardini, L., Novak, M., Piconcelli, E., Poggianti, B., Pomarede, D., Pompei, E., Ponman, T., Ceja, M. E. Ramos, Ranalli, P., Rapetti, D., Raychaudhury, S., Ricci, M., Rottgering, H., Sahlén, M., Sauvageot, J. -L., Schimd, C., Sereno, M., Smith, G. P., Umetsu, K., Valageas, P., Valotti, A., Valtchanov, I., Veropalumbo, A., Ascaso, B., Barnes, D., De Petris, M., Durret, F., Donahue, M., Ithana, M., Jarvis, M., Johnston-Hollitt, M., Kalfountzou, E., Kay, S., La Franca, F., Okabe, N., Muzzin, A., Rettura, A., Ricci, F., Ridl, J., Risaliti, G., Takizawa, M., Thomas, P., Truong, N., 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 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), University of Bristol [Bristol], Istituto Nazionale di Astrofisica (INAF), Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), INAF - Osservatorio Astronomico di Bologna (OABO), University of Michigan [Ann Arbor], University of Michigan System, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Department of Earth and Space Sciences [Göteborg], Chalmers University of Technology [Göteborg], 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), Anglo-Australian Observatory (AAO), Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), University of Liverpool, National Astronomical Observatory of Japan (NAOJ), Rheinische Friedrich-Wilhelms-Universität Bonn, Department of Physics [Thessaloniki], Aristotle University of Thessaloniki, Argelander-Institut für Astronomie (AlfA), University of Zagreb, NASA Goddard Space Flight Center (GSFC), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, University of Victoria [Canada] (UVIC), Istanbul University, European Space Astronomy Centre (ESAC), European Space Agency (ESA), INAF - Osservatorio Astronomico di Roma (OAR), Department of Physics [Oxford], University of Oxford [Oxford], Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, 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), 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), Indian Institute of Technology [Hyderabad] (IIT Hyderabad), University of Geneva [Switzerland], Uppsala University, INTEGRAL Science Data Center (ISDC), Geneva Observatory, University of Geneva [Switzerland]-University of Geneva [Switzerland], Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, Institute for Space Applications and Remote Sensing (ISARS/NOA), National Observatory of Athens (NOA), The University of Western Australia (UWA), University of Bologna, University of Chicago, University of Birmingham [Birmingham], CEA, DSM, SPP, Commissariat à l'énergie atomique et aux énergies alternatives (CEA), INAF - Osservatorio Astronomico di Padova (OAPD), European Southern Observatory (ESO), Lund University [Lund], University of Colorado [Boulder], Inter-University Centre for Astronomy and Astrophysics [Pune] (IUCAA), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Institut des Sciences Moléculaires d'Orsay (ISMO), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Academia Sinica Institute of Astronomy and Astrophysics (ASIAA), Academia Sinica, Service de Physique Théorique (SPhT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Jodrell Bank Centre for Astrophysics (JBCA), University of Manchester [Manchester], Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Yamagata University, Victoria University of Wellington, Roma Tre University, Hiroshima University, York University [Toronto], Department of Physics and Astronomy [Riverside], University of California [Riverside] (UCR), University of California-University of California, Caltech Department of Astronomy [Pasadena], California Institute of Technology (CALTECH), INAF - Osservatorio Astrofisico di Arcetri (OAA), University of Sussex, Università degli Studi di Roma Tor Vergata [Roma], Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), 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), Smithsonian Institution-Harvard University [Cambridge], Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), 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), Université Côte d'Azur (UCA), PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), National Observatory of Athens, Institute for Space Applications and Remote Sensing, 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), Jodrell Bank Centre for Astrophysics, Università degli Studi di Roma 'La Sapienza' [Rome], Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Pierre, M, Adami, C., Birkinshaw, M., Chiappetti, L., Ettori, S., Evrard, A., Faccioli, L., Gastaldello, F., Giles, P., Horellou, C., Iovino, A., Koulouridis, E., Lidman, C., Le Brun, A., Maughan, B., Maurogordato, S., Mccarthy, I., Miyazaki, S., Pacaud, F., Paltani, S., Plionis, M., Reiprich, T., Sadibekova, T., Smolcic, V., Snowden, S., Surdej, J., Tsirou, M., Vignali, C., Willis, J., Alis, S., Altieri, B., Baran, N., Benoist, C., Bongiorno, A., Bremer, M., Butler, A., Cappi, A., Caretta, C., Ciliegi, P., Clerc, N., Corasaniti, P.S., Coupon, J., Delhaize, J., Delvecchio, I., Democles, J., Desai, Sh., Devriendt, J., Dubois, Y., Eckert, D., Elyiv, A., Farahi, A., Ferraril, C., Fotopoulou, S., Forman, W., Georgantopoulos, I., Guglielmo, V., Huynh, M., Jerlin, N., Jones, Ch., Lavoie, S., Le Fevre, J.-P., Lieu, M., Kilbinger, M., Marulli, F., Mantz, A., Mcgee, S., Melin, J.-B., Melnyk, O., Moscardini, L., Novak, M., Piconcelli, E., Poggianti, B., Pomarede, D., Pompei, E., Ponman, T., Ramos Ceja, M.E., Rana, P., Rapetti, D., Raychaudhury, S., Ricci, M., Rottgering, H., Sahlen, M., Sauvageot, J.-L., Schimd, C., Sereno, M., Smith, G.P., Umetsu, K., Valageas, P., Valotti, A., Valtchanov, I., Veropalumbo, A., Ascaso, B., Barnes, D., De Petris, M., Durret, F., Donahue, M., Ithana, M., Jarvis, M., Johnston-Hollitt, M., Kalfountzou, E., Kay, S., La Franca, F., Okabe, N., Muzzin, A., Rettura, A., Ricci, F., Ridl, J., Risaliti, G., Takizawa, M., Thomas, P., Truong, N., Corasaniti, P. S., Desai, S. h., Jones, C. h., Le Fevre, J. P., Maruili, F., Melin, J. B., Ramos Ceja, M. E., Sauvageot, J. L., Smith, G. P., Johnston Hollitt, M., LA FRANCA, Fabio, Ricci, Federica, 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), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA), Agence Spatiale Européenne = European Space Agency (ESA), University of Oxford, Université de Genève = University of Geneva (UNIGE), Université de Genève = University of Geneva (UNIGE)-Université de Genève = University of Geneva (UNIGE), Harvard University-Smithsonian Institution, University of Bologna/Università di Bologna, Universiteit Leiden, 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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Università degli Studi Roma Tre = Roma Tre University (ROMA TRE), University of California [Riverside] (UC Riverside), and University of California (UC)-University of California (UC)
- Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] ,galaxies: active ,X-ray: general ,FOS: Physical sciences ,Astronomy and Astrophysic ,Astrophysics - Astrophysics of Galaxies ,XXL survey ,Space and Planetary Science ,galaxies: clusters: general ,Astrophysics of Galaxies (astro-ph.GA) ,active [galaxies] ,clusters: general [galaxies] ,cosmological parameter ,X-ray:general ,cosmological parameters ,general [X-ray] ,QC ,Astrophysics - Cosmology and Nongalactic Astrophysics ,QB - Abstract
The XXL survey currently covers two 25 sq. deg. patches with XMM observations of ~10ks. We summarise the scientific results associated with the first release of the XXL data set, that occurred mid 2016. We review several arguments for increasing the survey depth to 40 ks during the next decade of XMM operations. X-ray (z1 cluster density. It will eventually constitute a reference study and an ideal calibration field for the upcoming eROSITA and Euclid missions., Proceeding of the XMM Next Decade Workshop held at ESAC, 9-11 May 2016
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158. The Chandra COSMOS Legacy Survey: A New Window to the Obscured and Distant Universe
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Civano, Francesca M., Elvis, M., Hasinger, G., Comastri, A., Harrison, F., Urry, C. M., Brusa, M., Zamorani, G., Cappelluti, N., Scoville, N., Eva Schinnerer, Donley, J., Allevato, V., Silverman, J., Treister, E., Capak, P. L., Aldcroft, T. L., Alexander, D., D Abrusco, R., Finoguenov, A., Fruscione, A., Glikman, E., Hao, H., Jahnke, K., Karim, A., Kartaltepe, J. S., Leauthaud, A., Lanzuisi, G., Miyaji, T., Vignali, C., Fiore, F., Puccetti, S., Ranalli, P., Smolcic, V., Riguccini, L., Sargent, M., Schawinski, K., Stern, D., Gilli, R., Civano, Francesca M., Elvis, M., Hasinger, G., Comastri, A., Harrison, F., Urry, C. M., Brusa, M., Zamorani, G., Cappelluti, N., Scoville, N., Schinnerer, E., Donley, J., Allevato, V., Silverman, J., Treister, E., Capak, P. L., Aldcroft, T. L., Alexander, D., D'Abrusco, R., Finoguenov, A., Fruscione, A., Glikman, E., Hao, H., Jahnke, K., Karim, A., Kartaltepe, J. S., Leauthaud, A., Lanzuisi, G., Miyaji, T., Vignali, C., Fiore, F., Puccetti, S., Ranalli, P., Smolcic, V., Riguccini, L., Sargent, M., Schawinski, K., Stern, D., and Gilli, R.
- Abstract
The equatorial 2 deg2 COSMOS area is the only large field for which a complete, deep, pan-chromatic data set exists, from an outstanding survey effort, and that all large telescopes can observe. Now, this pioneering and ambitious COSMOS survey is undergoing major extension, pushing its frontiers via the newly approved Chandra COSMOS Legacy Survey, the second largest Chandra proposal ever approved.'COSMOS-Legacy' will uniformly cover the 1.7 deg2 COSMOS/HST field with 2.8 Ms of Chandra ACIS-I imaging at ~160 ksec depth. This project expands the current deep C-COSMOS area by a factor of ~3 at ~3e-16 (1.45 vs 0.44 deg2). This will be achieved with 56x50 ks tiles covering a total area of 2.2 deg2, which will be observed during Chandra Cycle 14. The area and depth of COSMOS Legacy are designed to detect ~40 z>4, and ~4 z>5 Large Scale Structures on >15 arcmin scales. These structures have proven to connect luminous AGN (over 200 at z>3 will be detected) and sub-mm galaxies. COSMOS Legacy will also probe mini-quasars at z>7, using anistotropies of the unresolved X-ray Background, and the masses of the Dark Matter halos hosting X-ray AGN up to 3, via autocorrelation functions on ~30arcmin scales. To fully achieve these goals, COSMOS Legacy is complemented by spectroscopic follow-up with DEIMOS and MOSFIRE at Keck and KMOS at the VLT and FMOS at Subaru, just approved observations with Spitzer and JVLA, and with harder (5-80 keV) X-ray imaging with NuSTAR. In the near future, observations with Subaru HyperSuprimeCam (grizY) to r(AB)=28.2 are planned.
159. The infrared-radio correlation of star-forming galaxies is strongly M-star-dependent but nearly redshift-invariant since z similar to 4
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Delvecchio, I, Daddi, E, Sargent, MT, Jarvis, MJ, Elbaz, D, Jin, S, Liu, D, Whittam, IH, Algera, H, Carraro, R, D'Eugenio, C, Delhaize, J, Kalita, BS, Leslie, S, Molnar, DC, Novak, M, Prandoni, I, Smolcic, V, Ao, Y, Aravena, M, Bournaud, F, Collier, JD, Randriamampandry, SM, Randriamanakoto, Z, Rodighiero, G, Schober, J, White, SV, and Zamorani, G
- Subjects
radio continuum: galaxies ,galaxies: star formation ,galaxies: active ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,galaxies: evolution ,Astrophysics::Galaxy Astrophysics ,infrared: galaxies - Abstract
Over the past decade, several works have used the ratio between total (rest 8-1000 mu m) infrared and radio (rest 1.4 GHz) luminosity in star-forming galaxies (q(IR)), often referred to as the infrared-radio correlation (IRRC), to calibrate the radio emission as a star formation rate (SFR) indicator. Previous studies constrained the evolution of q(IR) with redshift, finding a mild but significant decline that is yet to be understood. Here, for the first time, we calibrate q(IR) as a function of both stellar mass (M-star) and redshift, starting from an M-star-selected sample of > 400 000 star-forming galaxies in the COSMOS field, identified via (NUV-r)/(r-J) colours, at redshifts of 0.1
160. A JVLA 10~degree^2 deep survey
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Jarvis, M, Bhatnagar, S, Bruggen, M, Ferrari, C, Heywood, I, Hardcastle, M, Murphy, E, Taylor, R, Smirnov, O, Simpson, C, Smolcic, V, Stil, J, and Heyden, K
- Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics::Galaxy Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
(Abridged)One of the fundamental challenges for astrophysics in the 21st century is finding a way to untangle the physical processes that govern galaxy formation and evolution. Given the importance and scope of this problem, the multi-wavelength astronomical community has used the past decade to build up a wealth of information over specific extragalactic deep fields to address key questions in galaxy formation and evolution. These fields generally cover at least 10square degrees to facilitate the investigation of the rarest, typically most massive, galaxies and AGN. Furthermore, such areal coverage allows the environments to be fully accounted for, thereby linking the single halo to the two-halo terms in the halo occupation distribution. Surveys at radio wavelengths have begun to lag behind those at other wavelengths, especially in this medium-deep survey tier. However, the survey speed offered by the JVLA means that we can now reach a point where we can begin to obtain commensurate data at radio wavelengths to those which already exists from the X-ray through to the far-infrared over ~10 square degrees. We therefore present the case for a 10 square degree survey to 1.5uJy at L-band in A or B Array, requiring ~4000 hours to provide census of star-formation and AGN-accretion activity in the Universe. For example, the observations will allow galaxies forming stars at 10Msolar/yr to be detected out to z~1 and luminous infrared galaxies (1000Msolar/yr to be found out to z~6. Furthermore, the survey area ensures that we will have enough cosmic volume to find these rare sources at all epochs. The bandwidth will allow us to determine the polarisation properties galaxies in the high-redshift Universe as a function of stellar mass, morphology and redshift., 18 pages, 6 figures. White Paper submitted to the call for Very Large Array Sky Surveys
161. Pathway to the Square Kilometre Array - The German White Paper
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Aharonian, F., Arshakian, T. G., Allen, B., Banerjee, R., Beck, R., Becker, W., Bomans, D. J., Breitschwerdt, D., Bruggen, M., Brunthaler, A., Catinella, B., Champion, D., Ciardi, B., Crocker, R., Avillez, M. A., Dettmar, R. J., Engels, D., Ensslin, T., Enke, H., Fieseler, T., Gizon, L., Hackmann, E., Hartmann, B., Henkel, C., Hoeft, M., Iapichino, L., Innes, D., James, C., Jasche, J., Jones, D., Kagramanova, V., Kauffmann, G., Keane, E., Kerp, J., Klockner, H. -R, Kokkotas, K., Kramer, M., Krause, M., Krupp, N., Kunz, J., Lammerzahl, C., Lee, K. J., List, M., Liu, K., Lobanov, A., Mann, G., Merloni, A., Middelberg, E., Niemeyer, J., Noutsos, A., Perlick, V., Reich, W., Richter, P., Roy, A., Saintonge, A., Schafer, G., Schaffner-Bielich, J., Schinnerer, E., Schleicher, D., Schneider, P., Schwarz, D. J., Sedrakian, A., Sesana, A., Smolcic, V., Solanki, S., Tuffs, R., Vetter, M., Weber, E., Jochen Weller, Wex, N., Wucknitz, O., and Zwaan, M.
162. HST/ACS Morphology of Lyman Alpha Emitters at Redshift 5.7 in the COSMOS Field
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Taniguchi, Y., Murayama, T., Scoville, N. Z., Sasaki, S. S., Nagao, T., Shioya, Y., Saito, T., Ideue, Y., Nakajima, A., Matsuoka, K., Sanders, D. B., Mobasher, B., Aussel, H., Capak, P., Salvato, M., Koekemoer, A., Carilli, C., Cimatti, A., Ellis, R. S., Bianca Garilli, Giavalisco, M., Ilbert, O., Impey, C. D., Kitzbichler, M. G., Le Fevre, O., Mccracken, H. J., Scarlata, C., Schinnerer, E., Smolcic, V., Tribiano, S., and Trump, J. R.
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Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,FOS: Physical sciences ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We present detailed morphological properties of Lyman alpha emitters (LAEs) at z~ 5.7 in the COSMOS field, based on {\it Hubble Space Telescope} Advanced Camera for Surveys (ACS) data. The ACS imaging in the F814W filter covered 85 LAEs of the 119 LAEs identified in the full two square degree field, and 47 LAEs of them are detected in the ACS images. Nearly half of them are spatially extended with a size larger than 0.15 arcsec (~0.88 kpc at z=5.7) up to 0.4 arcsec (~2.5 kpc at z=5.7). The others are nearly unresolved compact objects. Two LAEs show double-component structures, indicating interaction or merging of building components to form more massive galaxies. By stacking the ACS images of all the detected sources, we obtain a Sersic parameter of n~0.7 with a half-light radius of 0.13 arcsec (0.76 kpc), suggesting that the majority of ACS detected LAEs have not spheroidal-like but disk-like or irregular light profiles. Comparing ACS F814W magnitudes (I_814) with Subaru/Suprime-Cam magnitudes in the NB816, i', and z' bands, we find that the ACS imaging in the F814W band mainly probes UV continuum rather than Lyman alpha line emission. UV continuum sizes tend to be larger for LAEs with larger Ly\alpha emission regions as traced by the NB816 imaging. The non-detection of 38 LAEs in the ACS images is likely due to the fact that their surface brightness is even too low both in the UV continuum and Lyalpha emission. Estimating I_814 for the LAEs with ACS non-detection from the z' and NB816 magnitudes, we find that 16 of these are probably LAEs with a size larger than 0.15 arcsec in UV continuum. All these results suggest that our LAE sample contains systematically larger LAEs in UV continuum size than those previously studied at z~6., Comment: 71 pages, 18 figures. Accepted for pulication in ApJ. High resolution paper: http://cosmos.phys.sci.ehime-u.ac.jp/~murayama/COSMOS/cosmos-lae57-acs.pdf
163. VizieR Online Data Catalog: COSMOS: strong lens systems (Faure+, 2008)
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Faure, C., Kneib, J. -P, Covone, G., Tasca, L., Leauthaud, A., Capak, P., Jahnke, K., Smolcic, V., La Torre, S., Ellis, R., Finoguenov, A., Koekemoer, A., Le Fevre, O., Richard Massey, Mellier, Y., Refregier, A., Rhodes, J., Scoville, N., Schinnerer, E., Taylor, J., Waerbeke, L., and Walcher, J.
164. The VLA-COSMOS Survey: II. Source Catalog of the Large Project
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Carilli, C., Bondi, M., Ciliegi, P., Jahnke, K., Scoville, N., Aussel, H., Koekemoer, A., Bertoldi, F., Schinnerer, E., Fevre, O., Smolcic, V., Blain, A., Urry, C., and Impey, C.
- Abstract
49 pages, 18 figures; accepted for publication in the ApJS, COSMOS special issue. The data will be available from the COSMOS archive at IPAC/IRSA http://irsa.ipac.caltech.edu/Missions/cosmos.html, more information on the VLA-COSMOS survey can be found at http://www.mpia-hd.mpg.de/COSMOS/, full version available at http://www.mpia-hd.mpg.de/COSMOS/#paper The VLA-COSMOS large project is described and its scientific objective is discussed. We present a catalog of ~ 3,600 radio sources found in the 2deg^2 COSMOS field at 1.4 GHz. The observations in the VLA A and C configuration resulted in a resolution of 1.5'x1.4' and a mean rms noise of ~ 10.5(15) uJy/beam in the central 1(2)deg^2. 80 radio sources are clearly extended consisting of multiple components, and most of them appear to be double-lobed radio galaxies. The astrometry of the catalog has been thoroughly tested and the uncertainty in the relative and absolute astrometry are 130mas and
165. The COSMOS2015 catalog (Laigle+, 2016)
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Laigle, C., Mccracken, H. J., Ilbert, O., Hsieh, B. C., Davidzon, I., Capak, P., Hasinger, G., Silverman, J. D., Pichon, C., Coupon, J., Aussel, H., Le Borgne, D., Caputi, K., Cassata, P., Y Chang, Y., Civano, F., Dunlop, J., Johan Fynbo, Kartaltepe, J. S., Koekemoer, A., Le Fevre, O., E. Le Floc'h, Leauthaud, A., Lilly, S., Lin, L., Marchesi, S., Bo Milvang-Jensen, Salvato, M., Sanders, D. B., Scoville, N., Smolcic, V., Mikkel Stockmann, Taniguchi, Y., Tasca, L., Sune Toft, Vaccari, M., and Zabl, J.
166. VizieR Online Data Catalog: COSMOS field Ly{alpha} emitters at z~5.7 (Murayama+, 2007)
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Murayama, T., Taniguchi, Y., Scoville, N. Z., Ajiki, M., Sanders, D. B., Mobasher, B., Aussel, H., Capak, P., Anton Koekemoer, Shioya, Y., Nagao, T., Carilli, C., Ellis, R. S., Garilli, B., Giavalisco, M., Kitzbichler, M. G., Le Fevre, O., Maccagni, D., Schinnerer, E., Smolcic, V., Tribiano, S., Cimatti, A., Komiyama, Y., Miyazaki, S., Sasaki, S. S., Koda, J., and Karoji, H.
167. THE COSMOS2015 CATALOG: EXPLORING THE 1 \textless z \textless 6 UNIVERSE WITH HALF A MILLION GALAXIES
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Hsieh, B., Lin, L., Ilbert, O., Civano, F., Toft, S., Mccracken, H., Leauthaud, A., Taniguchi, Y., Cassata, P., Silverman, J., Vaccari, Mattia, Marchesi, S., Capak, P., Dunlop, J., Kartaltepe, J., Lilly, S., Salvato, M., Le Borgne, D., Pichon, C., Le Fevre, O., Smolcic, V., Fynbo, J., Le FlocH, E., Tasca, L., Sanders, D., Milvang-Jensen, B., Stockmann, M., Caputi, K., Aussel, H., Davidzon, I., Coupon, J., Zabl, J., Laigle, C., Scoville, N., Hasinger, G., Koekemoer, A., Chang, Y., Borgne, D., Fevre, O., FlocH, E., and Vaccari, M.
- Abstract
International audience We present the COSMOS2015(24) catalog, which contains precise photometric redshifts and stellar masses for more than half a million objects over the 2deg(2) COSMOS field. Including new YJHK(s) images from the UltraVISTA-DR2 survey, Y-band images from Subaru/Hyper-Suprime-Cam, and infrared data from the Spitzer Large Area Survey with the Hyper-Suprime-Cam Spitzer legacy program, this near-infrared-selected catalog is highly optimized for the study of galaxy evolution and environments in the early universe. To maximize catalog completeness for bluer objects and at higher redshifts, objects have been detected on a chi(2) sum of the YJHK(s) and z(++) images. The catalog contains similar to 6 x 10(5) objects in the 1.5 deg(2) UltraVISTA-DR2 region and similar to 1.5 x 10(5) objects are detected in the “ultra-deep stripes” (0.62 deg(2)) at K-s \textless= 24.7 (3 sigma, 3 `, AB magnitude). Through a comparison with the zCOSMOS-bright spectroscopic redshifts, we measure a photometric redshift precision of sigma(Delta z(1) (+ zs)) = 0.007 and a catastrophic failure fraction of eta = 0.5%. At 3 \textless z \textless 6, using the unique database of spectroscopic redshifts in COSMOS, we find sigma(Delta z(1) (+ zs)) = 0.021 and eta = 13.2%. The deepest regions reach a 90% completeness limit of 10(10)M(circle dot) to z = 4. Detailed comparisons of the color distributions, number counts, and clustering show excellent agreement with the literature in the same mass ranges. COSMOS2015 represents a unique, publicly available, valuable resource with which to investigate the evolution of galaxies within their environment back to the earliest stages of the history of the universe. The COSMOS2015 catalog is distributed via anonymous ftp and through the usual astronomical archive systems (CDS, ESO Phase 3, IRSA).
168. A Second Stellar Color Locus: a Bridge from White Dwarfs to M stars
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Smolcic, V., Ivezic, Z., Knapp, G. R., Lupton, R. H., Pavlovski, K., Ilijic, S., Schlegel, D., J. Allyn Smith, Mcgehee, P. M., Silvestri, N. M., Hawley, S. L., Rockosi, C., Gunn, J. E., Strauss, M. A., Hilditch, R. W., Hensberge, H., and Pavlovski, K.
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Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Sloan Digital Sky Survey ,white dwarfs ,M dwarfs ,close binaries ,Astrophysics::Galaxy Astrophysics - Abstract
We report the discovery of a locus of stars in the SDSS $g-r$ vs. $u-g$ color-color diagram that connects the colors of white dwarfs and M dwarfs. While its contrast with respect to the main stellar locus is only $\sim$1:2300, this previously unrecognized feature includes 863 stars from SDSS Data Release 1. The position and shape of the feature is in good agreement with predictions of a simple binary star model that consists of a white dwarf and an M dwarf, with the components' luminosity ratio controlling the position along this binary system locus. SDSS DR1 spectra for 47 of these objects strongly support this model.
169. A Comparison of Photometric Redshift Techniques for Large Radio Surveys
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Norris, Ray P., Salvato, M., Longo, G., Brescia, M., Budavari, T., Carliles, S., Cavuoti, S., Farrah, D., Geach, J., Luken, K., Musaeva, A., Polsterer, K., Riccio, G., Seymour, N., Smolcic, V., Vaccari, M., and Zinn, P.
- Abstract
Future radio surveys will generate catalogs of tens of millions of radio sources, for which redshift estimates will be essential to achieve many of the science goals. However, spectroscopic data will be available for only a small fraction of these sources, and in most cases even the optical and infrared photometry will be of limited quality. Furthermore, radio sources tend to be at higher redshift than most optical sources (most radio surveys have a median redshift greater than 1) and so a significant fraction of radio sources hosts differ from those for which most photometric redshift templates are designed. We therefore need to develop new techniques for estimating the redshifts of radio sources. As a starting point in this process, we evaluate a number of machine-learning techniques for estimating redshift, together with a conventional template-fitting technique. We pay special attention to how the performance is affected by the incompleteness of the training sample and by sparseness of the parameter space or by limited availability of ancillary multiwavelength data. As expected, we find that the quality of the photometric-redshift degrades as the quality of the photometry decreases, but that even with the limited quality of photometry available for all-sky-surveys, useful redshift information is available for the majority of sources, particularly at low redshift. We find that a template-fitting technique performs best in the presence of high-quality and almost complete multi-band photometry, especially if radio sources that are also X-ray emitting are treated separately, using specific templates and priors. When we reduced the quality of photometry to match that available for the EMU all-sky radio survey, the quality of the template-fitting degraded and became comparable to some of the machine-learning methods. Machine learning techniques currently perform better at low redshift than at high redshift, because of incompleteness of the currently available training data at high redshifts.
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- 2019
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170. Properties and environment of radio-emitting galaxies in the VLA-zCOSMOS survey*
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Bardelli, S., Schinnerer, E., Smolcic, V., Zamorani, G., Zucca, E., Mignoli, M., Halliday, C., Kovac, K., Ciliegi, P., Caputi, K., Koekemoer, A. M., Bongiorno, A., Bondi, M., Bolzonella, M., Vergani, D., Pozzetti, L., Carollo, C. M., Contini, T., Kneib, J.-P., Le Fèvre, O., Lilly, S., Mainieri, V., Renzini, A., Scodeggio, M., Coppa, G., Cucciati, O., de la Torre, S., de Ravel, L., Franzetti, P., Garilli, B., Iovino, A., Kampczyk, P., Knobel, C., Lamareille, F., Le Borgne, J.-F., Le Brun, V., Maier, C., Pellò, R., Peng, Y., Perez-Montero, E., Ricciardelli, E., Silverman, J. D., Tanaka, M., Tasca, L., Tresse, L., Abbas, U., Bottini, D., Cappi, A., Cassata, P., Cimatti, A., Guzzo, L., Leauthaud, A., Maccagni, D., Marinoni, C., McCracken, H. J., Memeo, P., Meneux, B., Oesch, P., Porciani, C., Scaramella, R., Capak, P., Sanders, D., Scoville, N., Taniguchi, Y., and Jahnke, K.
- Abstract
Aims. We investigate the properties and the environment of radio sources with optical counterparts from the combined VLA-COSMOS and zCOSMOS samples. The advantage of this sample is the availability of optical spectroscopic informations, high quality redshifts, and accurate density determination.Methods. By comparing the star formation rates estimated from the optical spectral energy distribution with those based on the radio luminosity, we divide the radio sources in to three families passive AGN, non-passive AGN, and star-forming galaxies. These families occupy specific regions of the 8.0-4.5 µm infrared color- specific star-formation plane, from which we extract the corresponding control samples.Results. Only the passive AGN have a significantly different environmental distribution from their control sample. The fraction of radio-loud passive AGN increases from ~2% in underdense regions to ~15% for overdensities (1 + d) greater than 10. This trend is also present as a function of richness of the groups hosting the radio sources. Passive AGN in overdensities tend to have higher radio luminosities than those in lower density environments. Since the black hole mass distribution is similar in both environments, we speculate that, for low radio luminosities, the radio emission is controlled (by fuel availability or confinement of the radio jet by local gas pressure) by the interstellar medium of the host galaxy, while in other cases it is determined by the structure (group or cluster) in which the galaxy resides.
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- 2010
171. Distant star formation in the faint radio sky
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Algera, H.S.B., Röttgering, H.J.A., Hodge, J.A., Viti, S., Werf, P.P. van der, Smail, I., Smolcic, V., Bouwens, R.J., Riechers, D., and Leiden University
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Galaxy formation ,High redshift ,Astrophysics::High Energy Astrophysical Phenomena ,Galaxy evolution ,Star formation ,Active Galactic Nuclei ,Starburst galaxies ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Radio astronomy ,Astrophysics::Galaxy Astrophysics - Abstract
One of the key quests in astronomy is to study the growth and evolution of galaxies across cosmic time. Radio observations provide a powerful means of studying the formation of stars and subsequent buildup of distant galaxies, in a way that is unbiased by the presence of dust. This thesis provides a detailed view of faint, star-forming galaxies in the early Universe through sensitive radio observations, and compiles several studies probing distant star formation with both radio synchrotron and free-free emission. In Chapter 2, we detect a large number of galaxies using sensitive new radio data from the Very Large Array, allowing us to separate radio emission from star formation and active galactic nuclei in the faint radio sky. In Chapter 3, we calibrate synchrotron emission as a tracer of star formation in distant starburst galaxies, while in Chapters 4 & 5 we turn towards radio free-free emission — a faint but very powerful tracer of star formation. Using sensitive new radio data at high frequencies, we perform the first detailed studies of free-free emission in distant galaxies.
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- 2021
172. Radio selection of the most distant galaxy clusters
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R. T. Coogan, Ivan Delvecchio, Veronica Strazzullo, A. Calabrò, David Elbaz, Eva Schinnerer, Mark Sargent, Vernesa Smolčić, R. Gobat, Emanuele Daddi, Tao Wang, Chiara Ferrari, Francesco Valentino, Daizhong Liu, J. Delhaize, Mladen Novak, Qiusheng Gu, Shuowen Jin, 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), Joseph Louis LAGRANGE (LAGRANGE), 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), 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)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), 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), Daddi, E, Jin, S, Strazzullo, V, Sargent, Mt, Wang, T, Ferrari, C, Schinnerer, E, Smolcic, V, Calabro, A, Coogan, R, Delhaize, J, Delvecchio, I, Elbaz, D, Gobat, R, Gu, Q, Liu, D, Novak, M, Valentino, F, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), 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), Laboratoire AIM, Université Paris Diderot - Paris 7 ( UPD7 ) -Centre d'Etudes de Saclay, Joseph Louis LAGRANGE ( LAGRANGE ), Université Nice Sophia Antipolis ( 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 ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), and Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay
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Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Active galactic nucleus ,formation [galaxies] ,PRIRODNE ZNANOSTI. Fizika. Astronomija i astrofizika ,[ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph] ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,galaxies: high-redshift ,0103 physical sciences ,Galaxy formation and evolution ,Cluster (physics) ,galaxies: formation ,clusters: general [galaxies] ,NATURAL SCIENCES. Physics. Astronomy and Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysic ,010303 astronomy & astrophysics ,Galaxy cluster ,Astrophysics::Galaxy Astrophysics ,evolution [galaxies] ,QB ,Physics ,radio continuum: galaxies ,010308 nuclear & particles physics ,Star formation ,galaxies: clusters: general, galaxies: evolution, galaxies: formation, galaxies: high-redshift, radio continuum: galaxies ,Astronomy and Astrophysics ,Astrophysics - Astrophysics of Galaxies ,Galaxy ,First generation ,galaxies [radio continuum] ,Square degree ,galaxies: clusters: general ,galaxies: evolution ,Astrophysics - Cosmology and Nongalactic Astrophysics ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,galaxie [radio continuum] ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,high-redshift [galaxies] - Abstract
We show that the most distant X-ray detected cluster known to date, ClJ1001 at z=2.506, hosts a strong overdensity of radio sources. Six of them are individually detected (within 10") in deep 0.75" resolution VLA 3GHz imaging, with S(3GHz)>8uJy. Of the six, AGN likely affects the radio emission in two galaxies while star formation is the dominant source powering the remaining four. We searched for cluster candidates over the full COSMOS 2-square degree field using radio-detected 3GHz sources and looking for peaks in Sigma5 density maps. ClJ1001 is the strongest overdensity by far with >10sigma, with a simple z_phot>1.5 preselection. A cruder photometric rejection of z2.5. Samples of hundreds such high-redshift clusters could potentially constrain cosmological parameters and test cluster and galaxy formation models., ApJ Letters in press
- Published
- 2017
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173. A Comparison of Photometric Redshift Techniques for Large Radio Surveys
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James E. Geach, Giuseppe Longo, Kai Lars Polsterer, Ray P. Norris, Kieran J. Luken, Stefano Cavuoti, Vernesa Smolčić, Nick Seymour, Mattia Vaccari, Peter-Christian Zinn, Duncan Farrah, Giuseppe Riccio, Massimo Brescia, Tamás Budavári, Samuel Carliles, A. Musaeva, Mara Salvato, ITA, USA, GBR, DEU, AUS, Norris, R. P., Salvato, M., Longo, G., Brescia, M., Budavari, T., Carliles, S., Cavuoti, S., Farrah, D., Geach, J., Luken, K., Musaeva, A., Polsterer, K., Riccio, G., Seymour, N., Smolcic, V., Vaccari, M., and Zinn, P.
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techniques: photometric ,Galaxies ,radio sources ,Training set ,010504 meteorology & atmospheric sciences ,Computer science ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,01 natural sciences ,Galaxie ,Redshift ,Photometry (optics) ,Radio source ,Space and Planetary Science ,0103 physical sciences ,Astrophysics - Instrumentation and Methods for Astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,010303 astronomy & astrophysics ,Techniques: photometric ,0105 earth and related environmental sciences ,Photometric redshift - Abstract
Future radio surveys will generate catalogues of tens of millions of radio sources, for which redshift estimates will be essential to achieve many of the science goals. However, spectroscopic data will be available for only a small fraction of these sources, and in most cases even the optical and infrared photometry will be of limited quality. Furthermore, radio sources tend to be at higher redshift than most optical sources and so a significant fraction of radio sources hosts differ from those for which most photometric redshift templates are designed. We therefore need to develop new techniques for estimating the redshifts of radio sources. As a starting point in this process, we evaluate a number of machine-learning techniques for estimating redshift, together with a conventional template-fitting technique. We pay special attention to how the performance is affected by the incompleteness of the training sample and by sparseness of the parameter space or by limited availability of ancillary multi-wavelength data. As expected, we find that the quality of the photometric-redshift degrades as the quality of the photometry decreases, but that even with the limited quality of photometry available for all sky-surveys, useful redshift information is available for the majority of sources, particularly at low redshift. We find that a template-fitting technique performs best with high-quality and almost complete multi-band photometry, especially if radio sources that are also X-ray emitting are treated separately. When we reduced the quality of photometry to match that available for the EMU all-sky radio survey, the quality of the template-fitting degraded and became comparable to some of the machine learning methods. Machine learning techniques currently perform better at low redshift than at high redshift, because of incompleteness of the currently available training data at high redshifts., Comment: Submitted to PASP
- Published
- 2019
- Full Text
- View/download PDF
174. X-ray properties of radio-selected star forming galaxies in the Chandra-COSMOS survey
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I. Georgantopoulos, Eva Schinnerer, Piero Ranalli, Roberto Gilli, Andrea Comastri, Nico Cappelluti, Cristian Vignali, F. Civano, Vernesa Smolčić, Gianni Zamorani, Ranalli P., Comastri A., Zamorani G., Cappelluti N., Civano F., Georgantopoulos I., Gilli R., Schinnerer E., Smolcic V., and Vignali C.
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Brightness ,Radio Continuum: Galaxie ,Active galactic nucleus ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,010504 meteorology & atmospheric sciences ,Sample (material) ,Astrophysics::High Energy Astrophysical Phenomena ,galaxies: active ,FOS: Physical sciences ,galaxies [submillimeter] ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Star (graph theory) ,01 natural sciences ,Luminosity ,galaxies: high-redshift ,0103 physical sciences ,010303 astronomy & astrophysics ,galaxies: fundamental parameter ,Astrophysics::Galaxy Astrophysics ,0105 earth and related environmental sciences ,Physics ,starburst [galaxies] ,Astronomy and Astrophysics ,X-rays: galaxies ,radio continuum: galaxies ,galaxies: fundamental parameters ,galaxies: star formation ,Galaxy ,Redshift ,NATURAL SCIENCES. Physics ,PRIRODNE ZNANOSTI. Fizika ,Space and Planetary Science ,active [galaxies] ,Cosmos (category theory) ,distances and redshifts [galaxies] ,X-rays: galaxie ,high-redshift [galaxies] ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
X-ray surveys contain sizable numbers of star forming galaxies, beyond the AGN which usually make the majority of detections. Many methods to separate the two populations are used in the literature, based on X-ray and multiwavelength properties. We aim at a detailed test of the classification schemes and to study the X-ray properties of the resulting samples. We build on a sample of galaxies selected at 1.4 GHz in the VLA-COSMOS survey, classified by Smolcic et al. (2008) according to their optical colours and observed with Chandra. A similarly selected control sample of AGN is also used for comparison. We review some X-ray based classification criteria and check how they affect the sample composition. The efficiency of the classification scheme devised by Smolcic et al. (2008) is such that ~30% of composite/misclassified objects are expected because of the higher X-ray brightness of AGN with respect to galaxies. The latter fraction is actually 50% in the X-ray detected sources, while it is expected to be much lower among X-ray undetected sources. Indeed, the analysis of the stacked spectrum of undetected sources shows, consistently, strongly different properties between the AGN and galaxy samples. X-ray based selection criteria are then used to refine both samples. The radio/X-ray luminosity correlation for star forming galaxies is found to hold with the same X-ray/radio ratio valid for nearby galaxies. Some evolution of the ratio may be possible for sources at high redshift or high luminosity, tough it is likely explained by a bias arising from the radio selection. Finally, we discuss the X-ray number counts of star forming galaxies from the VLA- and C-COSMOS surveys according to different selection criteria, and compare them to the similar determination from the Chandra Deep Fields. The classification scheme proposed here may find application in future works and surveys., Comment: 15 pages, 7 figures, 3 tables
- Published
- 2012
175. First catalog of strong lens candidates in the COSMOS field
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Alexis Finoguenov, Alexie Leauthaud, Alexandre Refregier, Jean-Paul Kneib, Lidia Tasca, Anton M. Koekemoer, Sylvain de la Torre, Eva Schinnerer, Vernesa Smolčić, Jason Rhodes, Peter Capak, Yannick Mellier, C. Faure, Giovanni Covone, J. Walcher, Olivier Le Fevre, Ludovic Van Waerbeke, James E. Taylor, Nick Scoville, Richard S. Ellis, Richard Massey, Knud Jahnke, Astronomische Rechen-Institut [Heidelberg] (ARI), Zentrum für Astronomie der Universität Heidelberg (ZAH), Universität Heidelberg [Heidelberg] = Heidelberg University-Universität Heidelberg [Heidelberg] = Heidelberg University, 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), Istituto Nazionale di Fisica Nucleare, Sezione di Napoli (INFN, Sezione di Napoli), Istituto Nazionale di Fisica Nucleare (INFN), INAF - Osservatorio Astronomico di Capodimonte (OAC), Istituto Nazionale di Astrofisica (INAF), California Institute of Technology (CALTECH), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, AUTRES, Space Telescope Science Institute (STSci), Departement de Radioastronomie Millimétrique (DEMIRM), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), 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), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Department of Mathematics [Berkeley], University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Department of Physics and Astronomy [Leicester], University of Leicester, University of Toronto, Department of Physics [Toronto], Canadian Institute for Theoretical Astrophysics (CITA), Beaussier, Catherine, Universität Heidelberg [Heidelberg]-Universität Heidelberg [Heidelberg], Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), École normale supérieure - Paris (ENS Paris), California Institute of Technology (CALTECH)-NASA, University of California [Berkeley], University of California-University of California, Faure, C., Kneib, J. P., Covone, Giovanni, Tasca, L., Leauthaud, A., Capak, P., Jahnke, K., Smolcic, V., de la Torre, S., Ellis, R., Finoguenov, A., Koekemoer, A., Le Fevre, O., Massey, R., Mellier, Y., Refregier, A., Rhodes, J., Scoville, N., Schinnerer, E., Taylor, J., Van Waerbeke, L., and Walcher, J.
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Physics ,Structure formation ,Mass distribution ,010308 nuclear & particles physics ,Dark matter ,Astrophysics (astro-ph) ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Galaxy ,Cosmology ,law.invention ,Lens (optics) ,Gravitation ,[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] ,Space and Planetary Science ,law ,[PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] ,0103 physical sciences ,Halo ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics - Abstract
We present the first catalog of 67 strong galaxy-galaxy lens candidates discovered in the 1.64 square degree Hubble Space Telescope COSMOS survey. Twenty of these systems display multiple images or strongly curved large arcs. Our initial search is performed by visual inspection of the data and is restricted, for practical considerations, to massive early-type lens galaxies with arcs found at radii smaller than ~5''. Simple mass models are constructed for the best lens candidates and our results are compared to the strong lensing catalogs of the SLACS survey and the CASTLES database. These new strong galaxy-galaxy lensing systems constitute a valuable sample to study the mass distribution of early-type galaxies and their associated dark matter halos. We further expect this sample to play an important role in the testing of software algorithms designed to automatically search for strong gravitational lenses. From our analysis a robust lower limit is derived for the expected occurrence of strong galaxy-galaxy systems in current and future space-based wide-field imaging surveys. We expect that such surveys should uncover a large number of strong lensing systems (more than 10 systems per square degree), which will allow for a detailed statistical analysis of galaxy properties and will likely lead to constraints on models of gravitational structure formation and cosmology. The sample of strong lenses is available here: http://cosmosstronglensing.uni-hd.de/, 31 pages, 20 figures. Replaced Table 4, fig 18 and 19 (error found in the modeling code). Erratum accepted for publication in ApJ. No changes in content
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- 2008
176. The Chandra COSMOS Legacy survey: overview and point source catalog
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Meg Urry, Antonella Fruscione, Giorgio Lanzuisi, Heng Hao, Takamitsu Miyaji, Fiona A. Harrison, Nico Cappelluti, Andrea Comastri, Peter Capak, S. Marchesi, Günther Hasinger, Eva Schinnerer, Tom Aldcroft, Sune Toft, Daniel Stern, Jeyhan S. Kartaltepe, Alexander Karim, Cristian Vignali, Roberto Gilli, Vernesa Smolčić, Simonetta Puccetti, B. Trakhenbrot, F. Civano, Ezequiel Treister, N. J. Scoville, G. Zamorani, Knud Jahnke, Alexis Finoguenov, Mara Salvato, Martin Elvis, Marcella Brusa, Mark Sargent, K. Glotfelty, John D. Silverman, David M. Alexander, Viola Allevato, Fabrizio Fiore, Hermann Brunner, Stephanie M. LaMassa, Richard E. Griffiths, Piero Ranalli, Kevin Schawinski, ITA, USA, GBR, DEU, CHL, HRV, DNK, FIN, JPN, GRC, MEX, CHE, Civano, F., Marchesi, S., Comastri, A., Urry, M.C., Elvis, M., Cappelluti, N., Puccetti, S., Brusa, M., Zamorani, G., Hasinger, G., Aldcroft, T., Alexander, D.M., Allevato, V., Brunner, H., Capak, P., Finoguenov, A., Fiore, F., Fruscione, A., Gilli, R., Glotfelty, K., Griffiths, R.E., Hao, H., Harrison, F.A., Jahnke, K., Kartaltepe, J., Karim, A., Lamassa, S.M., Lanzuisi, G., Miyaji, T., Ranalli, P., Salvato, M., Sargent, M., Scoville, N.J., Schawinski, K., Schinnerer, E., Silverman, J., Smolcic, V., Stern, D., Toft, S., Trakhenbrot, B., Treister, E., Vignali, C., Department of Physics, Urry, M. C., Alexander, D. M., Griffiths, R. E., Harrison, F. A., Lamassa, S. M., and Scoville, N. J.
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ACTIVE GALACTIC NUCLEI ,catalog ,PRIRODNE ZNANOSTI. Fizika. Astronomija i astrofizika ,Point source ,catalogs ,cosmology: observations ,galaxies: evolution ,quasars: general ,surveys ,X-rays: general ,FOS: Physical sciences ,Astrophysics ,01 natural sciences ,X-RAY SURVEY ,general [X-rays] ,0103 physical sciences ,NATURAL SCIENCES. Physics. Astronomy and Astrophysics ,survey ,STRIPE 82 ,NUMBER COUNTS ,010303 astronomy & astrophysics ,evolution [galaxies] ,QB ,Physics ,EVOLUTION SURVEY COSMOS ,MS SOURCE CATALOGS ,XMM-NEWTON ,cosmology: observation ,general [quasars] ,010308 nuclear & particles physics ,Hardness ratio ,Astronomy and Astrophysics ,Limiting ,Astronomy and Astrophysic ,LOG S ,115 Astronomy, Space science ,Astrophysics - Astrophysics of Galaxies ,observations [cosmology] ,Large sample ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,BLACK-HOLE ,observation [cosmology] ,WIDE-FIELD SURVEY - Abstract
The COSMOS-Legacy survey is a 4.6 Ms Chandra program that has imaged 2.2 deg$^2$ of the COSMOS field with an effective exposure of $\simeq$160 ks over the central 1.5 deg$^2$ and of $\simeq$80 ks in the remaining area. The survey is the combination of 56 new observations, obtained as an X-ray Visionary Project, with the previous C-COSMOS survey. We describe the reduction and analysis of the new observations and the properties of 2273 point sources detected above a spurious probability of 2$\times 10^{-5}$. We also present the updated properties of the C-COSMOS sources detected in the new data. The whole survey includes 4016 point sources (3814, 2920 and 2440 in the full, soft and hard band). The limiting depths are 2.2 $\times$ 10$^{-16}$, 1.5 $\times$ 10$^{-15}$ and 8.9$\times$ 10$^{-16}$ ${\rm erg~cm}^{-2}~{\rm s}^{-1}$ in the 0.5-2, 2-10 and 0.5-10 keV bands, respectively. The observed fraction of obscured AGN with column density $> 10^{22}$ cm$^{-2}$ from the hardness ratio (HR) is $\sim$50$^{+17}_{-16}$%. Given the large sample, we compute source number counts in the hard and soft bands, significantly reducing the uncertainties of 5-10%. For the first time, we compute number counts for obscured (HR$>$-0.2) and unobscured (HR$, Comment: 20 pages, 16 figures, accepted for publication on ApJ on December 24, 2015
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177. Comparison of three different protocols for obtaining hemolysis.
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Nikolac Gabaj N, Miler M, Vrtaric A, Celap I, Bocan M, Filipi P, Radisic Biljak V, Simundic AM, Supak Smolcic V, and Kocijancic M
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- Hematologic Tests, Hemoglobins analysis, Humans, Serum chemistry, Hemolysis, Sodium
- Abstract
Objectives: Hemolysis is associated with erroneous or delayed results. Objectives of the study were to compare four different methods for obtaining hemolysis in vitro on three different analyzers., Methods: Hemolysis was prepared with addition of pure hemoglobin into serum pool, osmotic shock, aspiration through blood collection needle, freezing/thawing of whole blood. Biochemistry parameters were measured in duplicate at Architect c8000 (Abbott, Abbott Park, USA), Beckman Coulter AU680 (Beckman Coulter, Brea, USA) and Cobas 6000 c501 (Roche, Mannheim, Germany), according to manufacturers' declarations. Cut-off value was defined as the highest value of H index with corresponding bias lower than acceptance criteria., Results: We were not able to obtain results with freezing protocol. On all three platforms, lowest number of analytes were sensitive to hemolysis at H=0.5 using method of adding free hemoglobin. When osmotic shock was used, cut-off values for the most analytes were generally met at lower values. Hemolysis significantly interfered with measurement of potassium and lactate dehydrogenase (LD) at H=0.5 on all platforms. The most of the tested analytes had the lowest acceptable H index when aspiration method was used. At the low level of hemolysis (H=0.8) glucose, sodium, potassium, chloride, phosphate, and LD were affected on all analyzers, with some additional analytes depending on the manufacturer., Conclusions: Hemolysis interference differs on different analyzers and according to protocol for obtaining hemolysis. Aspiration method was generally the most sensitive to hemolysis interference, while addition of free Hb was the most resistant., (© 2022 Walter de Gruyter GmbH, Berlin/Boston.)
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- 2022
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178. Informed consent and ethics committee approval in laboratory medicine.
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Borovecki A, Mlinaric A, Horvat M, and Supak Smolcic V
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- Clinical Laboratory Techniques ethics, Ethics, Medical, Informed Consent
- Abstract
Informed consent is a process in which a human subject who is to participate in research needs to give his or her consent after being properly informed of the expected benefits as well as the potential harm of the research that will be performed. The function and purpose of the research ethics committee is to ensure that the research that will take place is in accordance with the relevant ethical standards. This means that the committee must assess the appropriateness of the design of the study reviewed. Research in the field of laboratory medicine has specific features, i.e. the use of samples that remain after routine analysis, data collection from databases containing patient information, data mining, collection of laboratory management data, method/instrument comparisons and validation, etc. As most of such research is either retrospective or not directly associated with patients, the question arises as to whether all types of research require informed consent and ethics committee approval. This article aims to clarify what is specific about obtaining informed consent and ethical approval in laboratory medicine, to provide general guidance on informed consent and ethical approval requirements based on the type of study, and what information should be included in applications for ethical approval and informed consent. This could also provide some guidance for future contributors to the Biochemia Medica., Competing Interests: Potential conflict of interest: None declared.
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- 2018
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179. An Analysis of Medical Laboratory Technology Journals' Instructions for Authors.
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Horvat M, Mlinaric A, Omazic J, and Supak-Smolcic V
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- Authorship standards, Ethics, Research, Journal Impact Factor, Medical Laboratory Science standards, Periodicals as Topic statistics & numerical data, Editorial Policies, Periodicals as Topic standards
- Abstract
Instructions for authors (IFA) need to be informative and regularly updated. We hypothesized that journals with a higher impact factor (IF) have more comprehensive IFA. The aim of the study was to examine whether IFA of journals indexed in the Journal Citation Reports 2013, "Medical Laboratory Technology" category, are written in accordance with the latest recommendations and whether the quality of instructions correlates with the journals' IF. 6 out of 31 journals indexed in "Medical Laboratory Technology" category were excluded (unsuitable or unavailable instructions). The remaining 25 journals were scored based on a set of 41 yes/no questions (score 1/0) and divided into four groups (editorial policy, research ethics, research integrity, manuscript preparation) by three authors independently (max score = 41). We tested the correlation between IF and total score and the difference between scores in separate question groups. The median total score was 26 (21-30) [portion of positive answers 0.63 (0.51-0.73)]. There was no statistically significant correlation between a journal's IF and the total score (rho = 0.291, P = 0.159). IFA included recommendations concerning research ethics and manuscript preparation more extensively than recommendations concerning editorial policy and research integrity (Ht = 15.91, P = 0.003). Some policies were poorly described (portion of positive answers), for example: procedure for author's appeal (0.04), editorial submissions (0.08), appointed body for research integrity issues (0.08). The IF of the "Medical Laboratory Technology" journals does not reflect a journals' compliance to uniform standards. There is a need for improving editorial policies and the policies on research integrity.
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- 2016
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180. Identification of authors without surnames: is ORCID the right way forward?
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Supak-Smolcic V, Simundic AM, and Lundberg GD
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- Humans, Biomedical Research, Peer Review, Research
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- 2016
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181. Biochemia Medica's editorial policy on authorship.
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Supak-Smolcic V and Simundic AM
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- Confidentiality, Humans, Negotiating, Research standards, Authorship standards, Editorial Policies, Periodicals as Topic standards
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Recent findings of authorship criteria violations in the manuscripts submitted to Biochemia Medica show that almost 40% of authors do not meet necessary criteria for authorship and thus indicate the need for better dissemination of editorial policy on authorship in our journal. We believe that such cases are mostly due to the authors' unawareness or the lack of understanding of the authorship criteria. With this article we therefore wish to declare our editorial policy on authorship and authorship criteria. Biochemia Medica endorses the authorship policy provided by the International Committee of Medical Journal Editors (ICMJE). Information on authorship is assessed by self-reported authorship claims during on-line manuscript submission. Those who meet ICMJE criteria shall be listed as authors, and all listed authors shall fulfill ICMJE criteria. All authors should be responsible for content of the article and have to know other authors' contributions to the study. Biochemia Medica will follow recommendations provided by Committee on Publication Ethics (COPE) flowcharts for possible disputes. By adhering to this procedure we hope to raise awareness about the importance of compliance with ICMJE authorship recommendations.
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- 2015
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182. Normalized MEDx chart as a useful tool for evaluation of analytical quality achievements. A picture is worth a thousand words.
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Supak Smolcic V and Bilic-Zulle L
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- Evaluation Studies as Topic, Reference Standards, Audiovisual Aids standards, Decision Trees
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- 2013
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183. The quality of the extra-analytical phase of laboratory practice in some developing European countries and Mexico - a multicentric study.
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Simundic AM, Bilic-Zulle L, Nikolac N, Supak-Smolcic V, Honovic L, Avram S, Beregovaja E, Dobreanu M, Guimaraes JT, Kovacs GL, Singh NM, Sierra-Amor RI, Sypniewska G, and Zima T
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- Adult, Aged, Clinical Laboratory Techniques standards, Europe, Female, Humans, Male, Mexico, Middle Aged, Phlebotomy statistics & numerical data, Quality Control, Research Design standards, Research Design statistics & numerical data, Self Report standards, Surveys and Questionnaires, Young Adult, Clinical Laboratory Techniques statistics & numerical data, Developing Countries statistics & numerical data
- Abstract
Background: This cross-sectional multicentric survey study aimed to assess the quality of the extra-analytical phase of laboratory activities in some developing European countries and Mexico. We assessed the quality of the extra-analytical practices in participating laboratories regarding the: a) sample acceptance criteria; b) phlebotomy procedures; c) test results reporting and d) recording non-conformities., Methods: A survey was performed during the April-May 2009. A total of 15 clinical laboratories from the following countries were included: Bosnia, Croatia, Czech Republic, Hungary, Mexico, Poland, Portugal, Romania, Serbia and Ukraine. Questions were scored (scores from 1-4) and average scores was calculated for each category., Results: The overall score for all respondents (n = 443) was 3.10 ± 0.33. The average score was 3.11 ± 0.56 for sample acceptance criteria, 2.76 ± 0.58 for phlebotomy and 3.34 ± 0.53, for test results reporting (F = 116.49; p < 0.001). Laboratory accreditation was associated with better practices and higher overall quality of the extra-analytical procedures (F = 16.62; p < 0.001). Moreover, the highest scores for sample acceptance criteria (F = 8.32; p < 0.001), phlebotomy procedures (F = 13.28; p < 0.001) and for reporting non-conformities (F = 33.62; p < 0.001) were observed for accredited laboratories or laboratories under preparation for accreditation., Conclusions: The overall quality of the extra-analytical practices in countries in this survey is not satisfactory. Phlebotomy practices are the most critical extra-analytical activity. Since laboratory accreditation was associated with better practices and higher overall quality of the extra-analytical procedures, we believe that the most significant improvement could be made by implementing the total quality management system and standardizing laboratory procedures.
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- 2011
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184. Validation of methods performance for routine biochemistry analytes at Cobas 6000 analyzer series module c501.
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Supak Smolcic V, Bilic-Zulle L, and Fisic E
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- Blood Proteins analysis, Cholesterol, HDL blood, Electrolytes blood, Enzymes blood, Humans, Immunoglobulin A blood, Immunoglobulin M blood, Reproducibility of Results, Trace Elements blood, Triglycerides blood, Chemistry, Clinical instrumentation, Chemistry, Clinical methods
- Abstract
Introduction: Cobas 6000 (Roche, Germany) is biochemistry analyzer for spectrophotometric, immunoturbidimetric and ion-selective determination of biochemical analytes. Hereby we present analytical validation with emphasis on method performance judgment for routine operation., Materials and Methods: Validation was made for 30 analytes (metabolites, enzymes, trace elements, specific proteins and electrolytes). Research included determination of within-run (N = 20) and between-run imprecision (N = 30), inaccuracy (N = 30) and method comparison with routine analyzer (Beckman Coulter AU640) (N = 50). For validation of complete analytical process we calculated total error (TE). Results were judged according to quality specification criteria given by European Working Group., Results: Within-run imprecision CVs were all below 5% except for cholesterol, triglycerides, IgA and IgM. Between-run CVs for all analytes were below 10%. Analytes that did not meet the required specifications for imprecision were: total protein, albumin, calcium, sodium, chloride, immunoglobulins and HDL cholesterol. Analytes that did not fulfill requirements for inaccuracy were: total protein, calcium, sodium and chloride. Analytes that deviated from quality specifications for total error were: total protein, albumin, calcium, sodium, chloride and IgM. Passing-Bablok regression analysis provided linear equation and 95% confidence interval for intercept and slope. Complete accordance with routine analyzer Beckman Coulter AU640 showed small number of analytes. Other analytes showed small proportional and/or small constant difference and therefore need to be adjusted for routine operation., Conclusions: Regarding low CV values, tested analyzer has satisfactory accuracy and precision and is extremely stable. Except for analytes that are coherent on both analyzers, some analytes require adjustments of slope and intercept for complete accordance.
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- 2011
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185. [Systematic bronchoscopy].
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OFNER E and SMOLCIC V
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- Humans, Bronchoscopy
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- 1956
186. [ON SOME DEVICES FOR AIR SAMPLING].
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SMOLCIC V
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- Air Pollution, Chemistry Techniques, Analytical
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- 1964
187. On the additional use of penicillin in the treatment of otogenous purulent meningitis.
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SMOLCIC V
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- Meningitis
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- 1947
188. Osteoma of the orbit of the frontal sinus.
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SASSO B and SMOLCIC V
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- Humans, Frontal Sinus, Neoplasms, Orbit, Osteoma, Paranasal Sinus Neoplasms
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- 1955
189. [The importance of pulmonary teams in our hospitals].
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OFNER E and SMOLCIC V
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- Humans, Hospitals, Lung Diseases
- Published
- 1954
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