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4 results on '"H. U. Norgaard-Nielsen"'

1. MIDIS: The Relation between Strong (Hβ + [O iii]) Emission, Star Formation, and Burstiness around the Epoch of Reionization

Author

K. I. Caputi, P. Rinaldi, E. Iani, P. G. Pérez-González, G. Östlin, L. Colina, T. R. Greve, H. U. Nørgaard-Nielsen, G. S. Wright, J. Álvarez-Márquez, A. Eckart, J. Hjorth, A. Labiano, O. Le Fèvre, F. Walter, P. van der Werf, L. Boogaard, L. Costantin, A. Crespo Gómez, S. Gillman, I. Jermann, D. Langeroodi, J. Melinder, F. Peissker, M. Güdel, Th. Henning, P. O. Lagage, and T. P. Ray

Subjects
Galaxy evolution, Reionization, Starburst galaxies, Astrophysics, QB460-466
Abstract

We investigate the properties of strong (H β + [O iii ]) emitters before and after the end of the “Epoch of Reionization” from z = 8 to z = 5.5. We make use of ultradeep JWST / NIRCam imaging in the parallel field (P2) of the MIRI Deep Imaging Survey (MIDIS) in the Hubble eXtreme Deep Field (H-XDF), in order to select prominent (H β + [O iii ]) emitters (with rest-frame equivalent width (EW _0 ) ≳ 100 Å) at z = 5.5–7, based on their flux density enhancement in the F356W band with respect to the spectral energy distribution continuum. We complement our selection with other (H β + [O iii ]) emitters from the literature at similar and higher ( z = 7−8) redshifts. We find (nonindependent) anticorrelations between EW _0 (H β + [O iii ]) and both galaxy stellar mass and age, in agreement with previous studies, and a positive correlation with specific star formation rate (sSFR). On the SFR– M ^⋆ plane, the (H β + [O iii ]) emitters populate both the star formation main sequence and the starburst region, which become indistinguishable at low stellar masses ( ${\mathrm{log}}_{10}({M}^{\star })\lt 7.5$ ). We find tentative evidence for a nonmonotonic relation between EW _0 (H β + [O iii ]) and SFR, such that both parameters correlate with each other at SFR ≳ 1 M _⊙ yr ^−1 , while the correlation flattens out at lower SFRs. This suggests that low metallicities producing high EW _0 (H β + [O iii ]) could be important at low SFR values. Interestingly, the properties of the strong emitters and other galaxies (33% and 67% of our z = 5.5–7 sample, respectively) are similar, including, in many cases, high sSFR. Therefore, it is crucial to consider both emitters and nonemitters to obtain a complete picture of the cosmic star formation activity around the Epoch of Reionization.

Published
2024
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2. INTERACTING SUPERNOVAE AND SUPERNOVA IMPOSTORS: SN 2009ip, IS THIS THE END?

Author

A. Pastorello, E. Cappellaro, C. Inserra, S. J. Smartt, G. Pignata, S. Benetti, S. Valenti, M. Fraser, K. Takxe1ts, S. Benitez, M. T. Botticella, J. Brimacombe, F. Bufano, F. Cellier-Holzem, M. T. Costado, G. Cupani, I. Curtis, N. Elias-Rosa, M. Ergon, J. P. U. Fynbo, F.-J. Hambsch, M. Hamuy, A. Harutyunyan, K. M. Ivarson, E. Kankare, J. C. Martin, R. Kotak, A. P. LaCluyze, K. Maguire, S. Mattila, J. Maza, M. McCrum, M. Miluzio, H. U. Norgaard-Nielsen, and M. C. Nysewander et al.

Published
2013

3. On the applicability of observatory corrections

Author

H. U. Norgaard-Nielsen

Subjects
Error analysis, Observatory, Statistics, Astronomy, Astrometry, Trigonometry, Parallax, Mathematics
Abstract

I have a few comments on the use of photometric parallaxes for examining the differences between the trigonometric parallaxes determined by different observatories. Dr. Lutz argues that because we don’t know the cause of the observatory corrections we should not use them in forming a new parallax catalogue. I have compared the trigonometric parallaxes with photometric parallaxes determined by means of the Strömgren four colour photometry (Nørgaard-Nielsen). My conclusion is that the observatory corrections applied in the Jenkins catalogue, especially the difference between the northern and the southern observatories, are significant. Dr. Upgren has recently reviewed the discussion of the observatory corrections and concludes that the north- south discrepancy is real. Therefore, I think that you have to apply observatory corrections in some way in the new catalogue, regardless of not having a satisfactory explanation for them.

Published
1978

4. Recent Developments in Astrophysical and Cosmological Exploitation of Microwave Surveys

Author

A. Mennella, Etienne Pointecouteau, Yoel Rephaeli, Carlo Burigana, L. Toffolatti, Marian Douspis, Michele Maris, Paolo de Bernardis, Silvia Masi, Rishi Khatri, Guo-Chin Liu, Paolo Natoli, Jacques Delabrouille, Francesco De Paolis, R. D. Davies, Hans Ulrik Nørgaard-Nielsen, C., Burigana, R. D., Davie, P., de Bernardi, J., Delabrouille, DE PAOLIS, Francesco, M., Douspi, R., Khatri, G. C., Liu, M., Mari, S., Masi, A., Mennella, P., Natoli, H. U., Norgaard Nielsen, E., Pointecouteau, Y., Rephaeli, L., Toffolatti, Ministerio de Economía y Competitividad (España), Agenzia Spaziale Italiana, Istituto Nazionale di Astrofisica, Ministero dell'Istruzione, dell'Università e della Ricerca, Agence Nationale de la Recherche (France), Dipartimento di Fisica [Roma La Sapienza], Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], 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), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), 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), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), 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), and 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)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Cosmic microwave background, FOS: Physical sciences, Galaxy clusters, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Cosmic background radiation, 01 natural sciences, 7. Clean energy, Cosmology, symbols.namesake, Cosmic infrared background, 0103 physical sciences, 14. Life underwater, Planck, Primordial galaxies, 010306 general physics, 010303 astronomy & astrophysics, Absolute zero, ComputingMilieux_MISCELLANEOUS, Mathematical Physics, Galaxy cluster, [PHYS]Physics [physics], Physics, COSMIC cancer database, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Zodiacal light, Milky Way, 13. Climate action, Space and Planetary Science, Active galaxies, symbols, Neutrino, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Microwave, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

arXiv:1302.3474v1.-- et al., In this paper, we focus on the astrophysical results and the related cosmological implications derived from recent microwave surveys, with emphasis to those coming from the Planck mission. We critically discuss the impact of systematic effects and the role of methods to separate the cosmic microwave background (CMB) signal from the astrophysical emissions and each different astrophysical component from the others. We then review the state-of-the-art diffuse emissions, extragalactic sources, cosmic infrared background and galaxy clusters, addressing the information they provide to our global view of the cosmic structure evolution and for some crucial physical parameters, as the neutrino mass. Finally, we present three different kinds of scientific perspectives for fundamental physics and cosmology offered by the analysis of on-going and future CMB projects at different angular scales dedicated to anisotropies in total intensity and polarization and to absolute temperature. © 2013 World Scientific Publishing Company., CB, MM, AM, PN acknowledge support by ASI through ASI/INAF Agreement I/072/09/0 for the Planck LFI Activity of Phase E2 and by MIUR through PRIN 2009 grant n. 2009XZ54H2. EP acknowledges the support of ANR project Multiverse under grant ANR-11-BD56-015. LT acknowledges partial financial support from the Spanish Ministerio de Economía y Competitividad, under proyects AYA2010-21766-C03-01, AYA2012-39475-C02-01 and by the Consolider Ingenio-2010 Programme, project CSD2010-00064.

Published
2013

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