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10 results on '"La Vieuville, G."'

1. MUSE observations towards the lensing cluster A2744: Intersection between the LBG and LAE populations at z $\sim$ 3-7

Author

de La Vieuville, G., Pelló, R., Richard, J., Mahler, G., Lévêque, L., Bauer, F. E., Lagattuta, D. J., Blaizot, J., Contini, T., Guaita, L., Kusakabe, H., Laporte, N., Martinez, J., Maseda, M. V., Schaerer, D., Schmidt, K. B., and Verhamme, A.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present a study of the intersection between the populations of star forming galaxies (SFGs) selected as either Lyman break galaxies (LBGs) or Lyman-alpha emitters (LAEs) in the redshift range 2.9 - 6.7, within the same volume of universe sampled by the Multi-Unit Spectroscopic Explorer (MUSE) behind the Hubble Frontier Fields lensing cluster A2744. We define three samples of star-forming galaxies: LBG galaxies with an LAE counterpart (92 galaxies), LBG galaxies without LAE counterpart (408 galaxies) and LAE galaxies without an LBG counterpart (46 galaxies). All these galaxies are intrinsically faint due to the lensing nature of the sample (Muv $\ge$ -20.5). The fraction of LAEs among all selected SFGs increases with redshift up to z $\sim$ 6 and decreases for higher redshifts. The evolution of LAE/LBG populations with UV magnitude and Lya luminosity shows that the LAE selection is able to identify intrinsically UV faint galaxies with Muv $\ge$ -15 that are typically missed in the deepest lensing photometric surveys. The LBG population seems to fairly represent the total population of SFGs down to Muv$\sim$-15. Galaxies with Muv$<-17$ tend to have SFRLya$<$SFRuv, whereas the opposite trend is observed within our sample for faint galaxies with Muv$>-17$, including galaxies only detected by their Lya emission, with a large scatter. These trends, previously observed in other samples of SFGs at high-$z$, are seen here for very faint Muv$\sim -15$ galaxies, much fainter than in previous studies. There is no clear evidence, based on the present results, for an intrinsic difference on the properties of the two populations selected as LBG and/or LAE. The observed trends could be explained by a combination of several facts, like the existence of different star-formation regimes, the dust content, the relative distribution and morphology of dust and stars, or the stellar populations

Published
2020
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2. Faint end of the $z \sim 3-7$ luminosity function of Lyman-alpha emitters behind lensing clusters observed with MUSE

Author

de La Vieuville, G., Bina, D., Pello, R., Mahler, G., Richard, J., Drake, A. B., Herenz, E. C., Bauer, F. E., Clément, B., Lagattuta, D., Laporte, N., Martinez, J., Patriìcio, V., Wisotzki, L., Zabl, J., Bouwens, R. J., Contini, T., Garel, T., Guiderdoni, B., Marino, R. A., Maseda, M. V., Matthee, J., Schaye, J., and Soucail, G.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present the results obtained with VLT/MUSE on the faint-end of the Lyman-alpha luminosity function (LF) based on deep observations of four lensing clusters. The precise aim of the present study is to further constrain the abundance of Lyman-alpha emitters (LAEs) by taking advantage of the magnification provided by lensing clusters. We blindly selected a sample of 156 LAEs, with redshifts between $2.9 \le z \le 6.7$ and magnification-corrected luminosities in the range $ 39 \lesssim \log L_{Ly_{\alpha}}$ [erg s$^{-1}$] $\lesssim 43$. The price to pay to benefit from magnification is a reduction of the effective volume of the survey, together with a more complex analysis procedure. To properly take into account the individual differences in detection conditions (including lensing configurations, spatial and spectral morphologies) when computing the LF, a new method based on the 1/Vmax approach was implemented. The LAE LF has been obtained in four different redshift bins with constraints down to $\log L_{Ly_{\alpha}} = 40.5$. From our data only, no significant evolution of LF mean slope can be found. When performing a Schechter analysis including data from the literature to complete the present sample a steep faint-end slope was measured varying from $\alpha = -1.69^{+0.08}_{-0.08}$ to $\alpha = -1.87^{+0.12}_{-0.12}$ between the lowest and the highest redshift bins. The contribution of the LAE population to the star formation rate density at $z \sim 6$ is $\lesssim 50$% depending on the luminosity limit considered, which is of the same order as the Lyman-break galaxy (LBG) contribution. The evolution of the LAE contribution with redshift depends on the assumed escape fraction of Lyman-alpha photons, and appears to slightly increase with increasing redshift when this fraction is conservatively set to one. (abridged), Comment: 32 pages, 22 figures

Published
2019
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4. Probing the faint-end luminosity function of Lyman-alpha emitters at 3 < z < 7 behind 17 MUSE lensing clusters

Author

Thai, T. T., primary, Tuan-Anh, P., additional, Pello, R., additional, Goovaerts, I., additional, Richard, J., additional, Claeyssens, A., additional, Mahler, G., additional, Lagattuta, D., additional, de la Vieuville, G., additional, Salvador-Solé, E., additional, Garel, T., additional, Bauer, F. E., additional, Jeanneau, A., additional, Clément, B., additional, and Matthee, J., additional

Published
2023
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5. Faint end of the z ∼ 3–7 luminosity function of Lyman-alpha emitters behind lensing clusters observed with MUSE

Author

De La Vieuville, G, Bina, D, Pello, R, Mahler, G, Richard, J, Drake, AB, Herenz, EC, Bauer, FE, Clément, B, Lagattuta, D, Laporte, N, Martinez, J, Patrício, V, Wisotzki, L, Zabl, J, Bouwens, RJ, Contini, T, Garel, T, Guiderdoni, B, Marino, RA, Maseda, MV, Matthee, J, Schaye, J, Soucail, G, de La Vieuville, G [0000-0002-4423-5835], and Apollo - University of Cambridge Repository

Subjects
5101 Astronomical Sciences, 51 Physical Sciences
Abstract

Contact. This paper presents the results obtained with the Multi-Unit Spectroscopic Explorer (MUSE) at the ESO Very Large Telescope on the faint end of the Lyman-alpha luminosity function (LF) based on deep observations of four lensing clusters. The goal of our project is to set strong constraints on the relative contribution of the Lyman-alpha emitter (LAE) population to cosmic reionization. Aims. The precise aim of the present study is to further constrain the abundance of LAEs by taking advantage of the magnification provided by lensing clusters to build a blindly selected sample of galaxies which is less biased than current blank field samples in redshift and luminosity. By construction, this sample of LAEs is complementary to those built from deep blank fields, whether observed by MUSE or by other facilities, and makes it possible to determine the shape of the LF at fainter levels, as well as its evolution with redshift. Methods. We selected a sample of 156 LAEs with redshifts between 2.9 ≤ z ≤ 6.7 and magnification-corrected luminosities in the range 39 ≲ log LLyα [erg s−1] ≲43. To properly take into account the individual differences in detection conditions between the LAEs when computing the LF, including lensing configurations, and spatial and spectral morphologies, the non-parametric 1/Vmax method was adopted. The price to pay to benefit from magnification is a reduction of the effective volume of the survey, together with a more complex analysis procedure to properly determine the effective volume Vmax for each galaxy. In this paper we present a complete procedure for the determination of the LF based on IFU detections in lensing clusters. This procedure, including some new methods for masking, effective volume integration and (individual) completeness determinations, has been fully automated when possible, and it can be easily generalized to the analysis of IFU observations in blank fields. Results. As a result of this analysis, the Lyman-alpha LF has been obtained in four different redshift bins: 2.9 < z < 6, 7, 2.9 < z < 4.0, 4.0 < z < 5.0, and 5.0 < z < 6.7 with constraints down to log LLyα = 40.5. From our data only, no significant evolution of LF mean slope can be found. When performing a Schechter analysis also including data from the literature to complete the present sample towards the brightest luminosities, a steep faint end slope was measured varying from α = −1.69−0.08+0.08 to α = −1.87−0.12+0.12 between the lowest and the highest redshift bins. Conclusions. The contribution of the LAE population to the star formation rate density at z ∼ 6 is ≲50% depending on the luminosity limit considered, which is of the same order as the Lyman-break galaxy (LBG) contribution. The evolution of the LAE contribution with redshift depends on the assumed escape fraction of Lyman-alpha photons, and appears to slightly increase with increasing redshift when this fraction is conservatively set to one. Depending on the intersection between the LAE/LBG populations, the contribution of the observed galaxies to the ionizing flux may suffice to keep the universe ionized at z ∼ 6.

Published
2020
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6. VizieR Online Data Catalog: 12 massive lensing clusters MUSE observations (Richard+, 2021)

Author

Richard, J., Claeyssens, A., Lagattuta, D., Guaita, L., Bauer, F. E., Pello, R., Carton, D., Bacon, R., Soucail, G., Prieto Lyon, G., Kneib, J. -P., Mahler, G., Clement, B., Mercier, W., Variu, A., Tamone, A., Ebeling, H., Schmidt, K. B., Nanayakkara, T., Maseda, M., Weilbacher, P. M., Bouché, N., Bouwens, R. J., Wisotzki, L., La Vieuville, G., Martinez, J., Patricio, V., Service de réanimation médicale [CHU Rouen], Hôpital Charles Nicolle [Rouen], CHU Rouen, Normandie Université (NU)-Normandie Université (NU)-CHU Rouen, Normandie Université (NU)-Normandie Université (NU)-Université de Rouen Normandie (UNIROUEN), Normandie Université (NU), Groupe de Recherche sur le Handicap Ventilatoire (GRHV), Normandie Université (NU)-Institute for Research and Innovation in Biomedicine (IRIB), Université de Rouen Normandie (UNIROUEN), Normandie Université (NU)-Normandie Université (NU)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Université de Rouen Normandie (UNIROUEN), Normandie Université (NU)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), Universidad Diego Portales [Santiago] (UDP), Departamento de Astronomía y Astrofísica [Santiago], Pontificia Universidad Católica de Chile (UC), 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), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), 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), Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), Deutsches Zentrum für Luft- und Raumfahrt (DLR), Astrophysikalisches Institut Potsdam (AIP), and Services communs OMP (UMS 831)

Subjects
Morphology, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Redshifts, Clusters: galaxy, Photometry: HST, ComputingMilieux_MISCELLANEOUS, Spectroscopy
Abstract

International audience

Published
2021

7. MUSE observations towards the lensing cluster A2744: Intersection between the LBG and LAE populations at z ∼ 3–7

Author

de La Vieuville, G., primary, Pelló, R., additional, Richard, J., additional, Mahler, G., additional, Lévêque, L., additional, Bauer, F. E., additional, Lagattuta, D. J., additional, Blaizot, J., additional, Contini, T., additional, Guaita, L., additional, Kusakabe, H., additional, Laporte, N., additional, Martinez, J., additional, Maseda, M. V., additional, Schaerer, D., additional, Schmidt, K. B., additional, and Verhamme, A., additional

Published
2020
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8. VizieR Online Data Catalog: LAE z\raisebox-0.5ex~3-7 luminosity functions (de La Vieuville+, 2019)

Author

La Vieuville, G., Bina, D., Pello, R., Mahler, G., Richard, J., Drake, A. B., Herenz, E. C., Bauer, F. E., Clement, B., Lagattuta, D., Laporte, N., Martinez, J., Patricio, V., Wisotzki, L., Zabl, J., Bouwens, R. J., Contini, T., Garel, T., Guiderdoni, B., Marino, R. A., Maseda, M. V., Matthee, J., Schaye, J., Soucail, G., Laboratoire d'Astrophysique de Marseille (LAM), and 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)

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Gravitational lensing, Clusters: galaxy
Published
2019

9. Faint end of the z similar to 3-7 luminosity function of Lyman-alpha emitters behind lensing clusters observed with MUSE

Author

de La Vieuville, G., Bina, D., Pello, R., Mahler, G., Richard, J., Drake, A. B., Herenz, Edmund Christian, Bauer, F. E., Clément, B., Lagattuta, D., Laporte, N., Martinez, J., Patrício, V., Wisotzki, L., Zabl, J., Bouwens, R. J., Contini, T., Garel, T., Guiderdoni, B., Marino, R. A., Maseda, M. V., Matthee, J., Schaye, J., Soucail, G., de La Vieuville, G., Bina, D., Pello, R., Mahler, G., Richard, J., Drake, A. B., Herenz, Edmund Christian, Bauer, F. E., Clément, B., Lagattuta, D., Laporte, N., Martinez, J., Patrício, V., Wisotzki, L., Zabl, J., Bouwens, R. J., Contini, T., Garel, T., Guiderdoni, B., Marino, R. A., Maseda, M. V., Matthee, J., Schaye, J., and Soucail, G.

Abstract

Contact. This paper presents the results obtained with the Multi-Unit Spectroscopic Explorer (MUSE) at the ESOVery Large Telescope on the faint end of the Lyman-alpha luminosity function (LF) based on deep observations of four lensing clusters. The goal of our project is to set strong constraints on the relative contribution of the Lyman-alpha emitter (LAE) population to cosmic reionization. Aims. The precise aim of the present study is to further constrain the abundance of LAEs by taking advantage of the magnification provided by lensing clusters to build a blindly selected sample of galaxies which is less biased than current blank field samples in redshift and luminosity. By construction, this sample of LAEs is complementary to those built from deep blank fields, whether observed by MUSE or by other facilities, and makes it possible to determine the shape of the LF at fainter levels, as well as its evolution with redshift. Methods. We selected a sample of 156 LAEs with redshifts between 2.9 <= z <= 6.7 and magnification-corrected luminosities in the range 39 less than or similar to log L-Ly alpha [erg s(-1)] less than or similar to 43. To properly take into account the individual differences in detection conditions between the LAEs when computing the LF, including lensing configurations, and spatial and spectral morphologies, the non-parametric 1/V-max method was adopted. The price to pay to benefit from magnification is a reduction of the effective volume of the survey, together with a more complex analysis procedure to properly determine the effective volume V-max for each galaxy. In this paper we present a complete procedure for the determination of the LF based on IFU detections in lensing clusters. This procedure, including some new methods for masking, effective volume integration and (individual) completeness determinations, has been fully automated when possible, and it can be easily generalized to the analysis of IFU observations in blank fields. Re

Published
2019
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10. Faint end of the z ∼ 3–7 luminosity function of Lyman-alpha emitters behind lensing clusters observed with MUSE

Author

de La Vieuville, G., primary, Bina, D., additional, Pello, R., additional, Mahler, G., additional, Richard, J., additional, Drake, A. B., additional, Herenz, E. C., additional, Bauer, F. E., additional, Clément, B., additional, Lagattuta, D., additional, Laporte, N., additional, Martinez, J., additional, Patrício, V., additional, Wisotzki, L., additional, Zabl, J., additional, Bouwens, R. J., additional, Contini, T., additional, Garel, T., additional, Guiderdoni, B., additional, Marino, R. A., additional, Maseda, M. V., additional, Matthee, J., additional, Schaye, J., additional, and Soucail, G., additional

Published
2019
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