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15 results on '"Floriane Leclercq"'

1. MUSEQuBES: calibrating the redshifts of Ly α emitters using stacked circumgalactic medium absorption profiles

Author

Martin Wendt, Jarle Brinchmann, Hsiao-Wen Chen, Sean D. Johnson, Michael V. Maseda, Johan Richard, Joop Schaye, Jorryt Matthee, Nicolas Bouché, T. Contini, Tanya Urrutia, Anne Verhamme, Sowgat Muzahid, Sebastiano Cantalupo, Johannes Zabl, Mohammad Akhlaghi, Raffaella Anna Marino, Adélaïde Claeyssens, Lutz Wisotzki, Floriane Leclercq, Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Department of Computer Science [ETH Zürich] (D-INFK), 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), Astrophysikalisches Institut Potsdam (AIP), Équipe de droit international, européen et comparé (EDIEC), Université Jean Moulin - Lyon 3 (UJML), Université de Lyon-Université de Lyon, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Universiteit Leiden, 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), 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), ANR-17-CE31-0017,3DGASFLOWS,Comprendre le rôle des écoulements de gaz autour des galaxies grâce à une confrontation entre observations 3D et simulations numériques(2017), Muzahid, S, Schaye, J, Marino, R, Cantalupo, S, Brinchmann, J, Contini, T, Wendt, M, Wisotzki, L, Zabl, J, Bouche, N, Akhlaghi, M, Chen, H, Claeyssens, A, Johnson, S, Leclercq, F, Maseda, M, Matthee, J, Richard, J, Urrutia, T, Verhamme, A, Météo-France -Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo-France -Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), and Leibniz-Institut für Astrophysik Potsdam (AIP)

Subjects
Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, Dark matter, Galaxies: high-redshift, Quasars: absorption lines, Astronomy and Astrophysics, Quasar, Astrophysics, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Galaxy, Redshift, Space and Planetary Science, haloes, Quasars: absorption lines [Galaxies], 0103 physical sciences, Emission spectrum, Halo, Galaxies: haloe, 010303 astronomy & astrophysics, Equivalent width
Abstract

Lyman$-\alpha$ (Ly$\alpha$) emission lines are typically found to be redshifted with respect to the systemic redshifts of galaxies, likely due to resonant scattering of Ly$\alpha$ photons. Here we measure the average velocity offset for a sample of 96 $z\approx3.3$ Ly$\alpha$ emitters (LAEs) with a median Ly$\alpha$ flux (luminosity) of $\approx 10^{-17}~\rm erg~cm^{-2}~s^{-1}$ ($\approx10^{42}~\rm erg~s^{-1}$) and a median star formation rate (SFR) of $\approx1.3 \rm M_{\odot} yr^{-1}$ (not corrected for possible dust extinction), detected by the Multi-Unit Spectroscopic Explorer as part of our MUSEQuBES circumgalactic medium (CGM) survey. By postulating that the stacked CGM absorption profiles of these LAEs, probed by 8 background quasars, must be centered on the systemic redshift, we measure an average velocity offset, V$_{\rm offset} = 171 \pm 8$ $\rm km s^{-1}$, between the Ly$\alpha$ emission peak and the systemic redshift. The observed V$_{\rm offset}$ is lower by factors of $\approx1.4$ and $\approx2.6$ compared to the velocity offsets measured for narrow-band selected LAEs and Lyman break galaxies, respectively, which probe galaxies with higher masses and SFRs. Consistent with earlier studies based on direct measurements for individual objects, we find that the V$_{\rm offset}$ is correlated with the full width at half-maximum of the red peak of the Ly$\alpha$ line, and anti-correlated with the rest-frame equivalent width. Moreover, we find that $V_{\rm offset}$ is correlated with SFR with a sub-linear scaling relation, V$_{\rm offset}\propto \rm SFR^{0.16\pm0.03}$. Adopting the mass scaling for main sequence galaxies, such a relation suggests that V$_{\rm offset}$ scales with the circular velocity of the dark matter halos hosting the LAEs., Comment: Published on 15 May, 2020 along with an erratum (Ref: MNRAS 498, 4424, 2020, doi:10.1093/mnras/staa2668), since Fig. 2 has not been updated in the published version. There are other typos in the published version, introduced by the typesetter, which cannot be revised in the erratum. We feel that the astrp-ph version is more accurate than the published one

Published
2020
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2. Recovery and analysis of rest-frame UV emission lines in 2052 galaxies observed with MUSE at 1.5 < z < 6.4

Author

Leindert Boogaard, Lutz Wisotzki, Valentin Mauerhofer, Roland Bacon, Joop Schaye, J. Kerutt, Wolfram Kollatschny, Tanya Urrutia, Michael V. Maseda, Kasper B. Schmidt, Thierry Contini, Simon Conseil, Guillaume Mahler, Edmund Christian Herenz, Floriane Leclercq, Johan Richard, Mirko Krumpe, Jorryt Matthee, Anna Feltre, Themiya Nanayakkara, Leibniz Institute for Astrophysics Potsdam (AIP), 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), Gemini Observatory [Southern Operations Center], Association of Universities for Research in Astronomy (AURA), 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), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), 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), and 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)

Subjects
Astrophysics - instrumentation and methods for astrophysics, Electron density, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics - astrophysics of galaxies, Astrophysics, Photoionization, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Spectral line, Methods: observational, 0103 physical sciences, Galaxy formation and evolution, Emission spectrum, Techniques: imaging spectroscopy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Line (formation), Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Galaxies: high-redshift, Astronomy and Astrophysics, Galaxy, Redshift, ISM: lines and bands, Galaxies: ISM, Space and Planetary Science, Ultraviolet: galaxies
Abstract

[Abbreviated] Rest-frame UV emission lines probe physical parameters of the emitting star-forming galaxies and their environments. The strongest main UV line, Ly$\alpha$, has been instrumental in advancing the general knowledge of galaxy formation in the early universe. However, observing Ly$\alpha$ emission becomes increasingly challenging at $z \gtrsim 6$ when the neutral hydrogen fraction of the CGM and IGM increases. Secondary weaker UV emission lines provide important alternative methods for studying galaxy properties at high redshift. We present a large sample of rest-frame UV emission line sources at intermediate redshift for calibrating and exploring the connection between secondary UV lines and the emitting galaxies' physical properties and their Ly$\alpha$ emission. The sample of 2052 emission line sources with $1.5 < z < 6.4$ was selected through untargeted source detection in three-dimensional MUSE data cubes. We searched optimally extracted 1D spectra of the full sample for UV emission features via emission line template matching, resulting in a sample of more than 100 rest-frame UV emission line detections. We show that the detection efficiency of (non-Ly$\alpha$) UV emission lines increases with survey depth, and that the UV emission line strength often correlate with the strength of Ciii]. We measured the velocity offsets of resonant emission lines with respect to systemic tracers as well as the electron density and the gas-phase abundance. Lastly, using "PhotoIonization Model Probability Density Functions" we find that the UV line emitters generally have ionization parameter log10(U) $\approx$ -2.5 and metal mass fractions that scatter around Z $\approx$ 10$^{-2}$, that is Z $\approx$ 0.66Z$\odot$. Value-added catalogs of the full sample of MUSE objects studied in this work and a collection of UV line emitters from the literature are provided with this paper., Comment: Accepted by A&A. Contains 54 pages, 21 figures, and appendices. Catalogs described in Tables B.1 and C.1 will be made available with published paper

Published
2021
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3. MusE GAs FLOw and Wind (MEGAFLOW) VIII. Discovery of a Mgii emission halo probed by a quasar sightline

Author

Jarle Brinchmann, Nicolas Bouché, Sowgat Muzahid, Johannes Zabl, Thierry Contini, Joop Schaye, Floriane Leclercq, Johan Richard, Ilane Schroetter, Martin Wendt, Lutz Wisotzki, Roland Bacon, Sebastiano Cantalupo, Thibault Garel, Zabl, J, Bouche, N, Wisotzki, L, Schaye, J, Leclercq, F, Garel, T, Wendt, M, Schroetter, I, Muzahid, S, Cantalupo, S, Contini, T, Bacon, R, Brinchmann, J, Richard, J, 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), Saint Mary's University [Halifax], Leibniz-Institut für Astrophysik Potsdam (AIP), Leiden Observatory [Leiden], Universiteit Leiden, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), 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), ANR-17-CE31-0017,3DGASFLOWS,Comprendre le rôle des écoulements de gaz autour des galaxies grâce à une confrontation entre observations 3D et simulations numériques(2017), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Universiteit Leiden [Leiden], 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), and 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)

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics - astrophysics of galaxies, evolution, galaxies: haloes, intergalactic medium, quasars: absorption lines, quasars: individual: SDSSJ0937 + 0656 [galaxies], FOS: Physical sciences, quasars: absorption line, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Luminosity, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], galaxies: haloe, 0103 physical sciences, Absorption (logic), Surface brightness, Continuum (set theory), Galaxies: haloes, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Quasars: absorption lines, Astronomy and Astrophysics, Quasar, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), quasars: individual: SDSSJ0937 + 0656, Halo, Impact parameter, galaxies: evolution
Abstract

Using deep (11.2hr) VLT/MUSE data from the MEGAFLOW survey, we report the first detection of extended MgII emission from a galaxy's halo that is probed by a quasar sightline. The MgII $\lambda\lambda$ 2796,2803 emission around the $z = 0.702$ galaxy ($\log(M_*/\mathrm{M_\odot}) = 10.05^{+0.15}_{-0.11}$) is detected out to $\approx$25 kpc from the central galaxy and covers $1.0\times10^3$ kpc$^2$ above a surface brightness of $14\times10^{-19} \mathrm{erg} \mathrm{s}^{-1} \mathrm{cm}^{-2}\,\mathrm{arcsec}^{-2}$ ($2 \sigma$; integrated over 1200 km s$^{-1}$ =19A and averaged over $1.5 \;\mathrm{arcsec}^2$). The MgII emission around this highly inclined galaxy ($\simeq$75 deg) is strongest along the galaxy's projected minor axis, consistent with the MgII gas having been ejected from the galaxy into a bi-conical structure. The quasar sightline, which is aligned with the galaxy's minor axis, shows strong MgII $\lambda$2796 absorption (EW$_0$ = 1.8A) at an impact parameter of 39kpc from the galaxy. Comparing the kinematics of both the emission and the absorption - probed with VLT/UVES -, to the expectation from a simple toy model of a bi-conical outflow, we find good consistency when assuming a relatively slow outflow ($v_\mathrm{out}= 130\;\mathrm{km}\,\mathrm{s}^{-1}$). We investigate potential origins of the extended MgII emission using simple toy models. With continuum scattering models we encounter serious difficulties in explaining the luminosity of the MgII halo and in reconciling density estimates from emission and absorption. Instead, we find that shocks might be a more viable source to power the extended MgII (and non-resonant [OII]) emission., Comment: Version as resubmitted to MNRAS after addressing referee's comments (24 pages, 18 figures)

Published
2021
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4. The MUSE Hubble Ultra Deep Field Survey. XIV. Evolution of the Ly α emitter fraction from z = 3 to z = 6

Author

Takuya Hashimoto, Roland Bacon, Thibault Garel, Jeremy Blaizot, Roser Pello, Alyssa B. Drake, Raffaella Anna Marino, Josephine Kerutt, Hanae Inami, Bruno Guiderdoni, Edmund Christian Herenz, Simon Conseil, Pascal Oesch, Joop Schaye, Guillaume Mahler, Michael V. Maseda, Anne Verhamme, Floriane Leclercq, Johan Richard, Kasper B. Schmidt, Haruka Kusakabe, Jorryt Matthee, 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), 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), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), and 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)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Population, first stars, FOS: Physical sciences, Astrophysics, 01 natural sciences, galaxies: high-redshift, 0103 physical sciences, Galaxy formation and evolution, dark ages, education, 010303 astronomy & astrophysics, Reionization, Physics, education.field_of_study, 010308 nuclear & particles physics, Astronomy and Astrophysics, early Universe, Hubble Ultra-Deep Field, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), cosmology: observations, Intergalactic travel, reionization, intergalactic medium, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Equivalent width, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Lya emitter (LAE) fraction, X_LAE, is a potentially powerful probe of the evolution of the intergalactic neutral hydrogen gas fraction. However, uncertainties in the measurement of X_LAE are still debated. Thanks to deep data obtained with MUSE, we can measure the evolution of X_LAE homogeneously over a wide redshift range of z~3-6 for UV-faint galaxies (down to M_1500~-17.75). This is significantly fainter than in former studies, and allows us to probe the bulk of the population of high-z star-forming galaxies. We construct a UV-complete photo-redshift sample following UV luminosity functions and measure the Lya emission with MUSE using the second data release from the MUSE HUDF Survey. We derive the redshift evolution of X_LAE for M_1500 in [-21.75;-17.75] for the first time with a equivalent width range EW(Lya)>=65 A and find low values of X_ LAE~50 A at z~3-4, in contrast with previous work. The differences in X_LAE mainly arise from selection biases for Lyman Break Galaxies (LBGs) in the literature: UV-faint LBGs are more easily selected if they have strong Lya emission, hence X_LAE is biased towards higher values. Our results suggest either a lower increase of X_LAE towards z~6 than previously suggested, or even a turnover of X_LAE at z~5.5, which may be the signature of a late or patchy reionization process. We compared our results with predictions from a cosmological galaxy evolution model. We find that a model with a bursty star formation (SF) can reproduce our observed X_LAE much better than models where SF is a smooth function of time., Comment: 25 pages, 17 figures, 5 tables, accepted for publication in A&A

Published
2020
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5. Spectral variations of Lyman alpha emission within strongly lensed sources observed with MUSE

Author

Thibault Garel, B. Clement, Anne Verhamme, Edmund Christian Herenz, David Carton, Jeremy Blaizot, Johan Richard, Vera Patrício, Rike Saust, Floriane Leclercq, Lutz Wisotzki, Joop Schaye, Roland Bacon, Raffaella Anna Marino, Sowgat Muzahid, Adélaïde Claeyssens, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, 010308 nuclear & particles physics, FOS: Physical sciences, gravitational lensing: strong, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Galaxy, Space and Planetary Science, galaxies: high-redshift, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), strong [gravitational lensing], 0103 physical sciences, ultraviolet: galaxies, Alpha decay, galaxies [ultraviolet], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, high-redshift [galaxies]
Abstract

We present an analysis of HI Lyman-alpha emission in deep VLT/MUSE observations of two highly magnified and extended galaxies at z=3.5 and 4.03, including a newly discovered, almost complete Einstein ring. While these Lyman-alpha haloes are intrinsically similar to the ones typically seen in other MUSE deep fields, the benefits of gravitational lensing allows us to construct exceptionally detailed maps of Lyman-alpha line properties at sub-kpc scales. By combining all multiple images, we are able to observe complex structures in the Lyman-alpha emission and uncover small (~ 120 km/s in Lyman-alpha peak shift), but significant at > 4 sigma, systematic variations in the shape of the Lyman-alpha line profile within each halo. Indeed, we observe a global trend for the line peak shift to become redder at large radii, together with a strong correlation between the peak wavelength and line width. This systematic intrahalo variation is markedly similar to the object-to-object variations obtained from the integrated properties of recent large samples. Regions of high surface brightness correspond to relatively small line shifts, which could indicate that Lyman-alpha emission escapes preferentially from regions where the line profile has been less severely affected by scattering of Lyman-alpha photons., 9 pages, 4 figures, accepted for publication in MNRAS

Published
2019
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6. The MUSE Hubble Ultra Deep Field Survey

Author

Michael V. Maseda, Leindert Boogaard, Laurence Tresse, Anne Verhamme, Kasper B. Schmidt, Hanae Inami, Haruka Kusakabe, Jorryt Matthee, Anna Feltre, Jeremy Blaizot, Peter M. Weilbacher, Johan Richard, Jayadev Pradeep, Floriane Leclercq, Jarle Brinchmann, Sebastiano Cantalupo, Lutz Wisotzki, Raffaella Anna Marino, Joop Schaye, Tanya Urrutia, Takuya Hashimoto, Roland Bacon, David Carton, Wolfram Kollatschny, Themiya Nanayakkara, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), 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), Feltre, A, Maseda, M, Bacon, R, Pradeep, J, Leclercq, F, Kusakabe, H, Wisotzki, L, Hashimoto, T, Schmidt, K, Blaizot, J, Brinchmann, J, Boogaard, L, Cantalupo, S, Carton, D, Inami, H, Kollatschny, W, Marino, R, Matthee, J, Nanayakkara, T, Richard, J, Schaye, J, Tresse, L, Urrutia, T, Verhamme, A, and Weilbacher, P

Subjects
Stellar mass, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, medicine.disease_cause, ultraviolet: ISM, 01 natural sciences, Spectral line, galaxies: high-redshift, 0103 physical sciences, Ultraviolet: galaxie, medicine, Emission spectrum, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Line (formation), Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Hubble Ultra-Deep Field, Astrophysics - Astrophysics of Galaxies, ISM: lines and band, Redshift, Galaxy, ISM: lines and bands, Space and Planetary Science, ultraviolet: galaxies, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Ultraviolet, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We investigate the ultraviolet (UV) spectral properties of faint Lyman-$\alpha$ emitters (LAEs) in the redshift range 2.93. We compute various averaged spectra of LAEs sub-sampled on the basis of their observational (e.g., Ly$\alpha$ strength, UV magnitude and spectral slope) and physical (e.g., stellar mass and star-formation rate) properties. We search for UV spectral features other than Ly$\alpha$, such as higher-ionization nebular emission lines and absorption features. We successfully observe the OIII]1666 and CIII]909 collisionally excited emission lines and the HeII1640 recombination feature, as well as the resonant CIV1550 doublet either in emission or P-Cygni. We compare the observed spectral properties of the different mean spectra and find the emission lines to vary with the observational and physical properties of the LAEs. In particular, the mean spectra of LAEs with larger Ly$\alpha$ equivalent widths, fainter UV magnitudes, bluer UV spectral slopes and lower stellar masses show the strongest nebular emission. The line ratios of these lines are similar to those measured in the spectra of local metal-poor galaxies, while their equivalent widths are weaker compared to the handful of extreme values detected in individual spectra of z>2 galaxies. This suggests that weak UV features are likely ubiquitous in high z, low-mass and faint LAEs. We publicly release the stacked spectra as they can serve as empirical templates for the design of future observations, such as those with the James Webb Space Telescope and the Extremely Large Telescope., Comment: 26 pages, 18 figures. Accepted for publication in A&A

Published
2020
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7. The MUSE Hubble Ultra Deep Field Survey : XIII. Spatially resolved spectral properties of Lyman α haloes around star-forming galaxies at z > 3

Author

Raffaella Anna Marino, Gabriele Pezzulli, Thibault Garel, Edmund Christian Herenz, Jérémy Blaizot, Sebastiano Cantalupo, Floriane Leclercq, Anne Verhamme, Lutz Wisotzki, Adélaïde Claeyssens, Kasper B. Schmidt, Haruka Kusakabe, Takuya Hashimoto, Simon Conseil, Peter D. Mitchell, Jorryt Matthee, Michael V. Maseda, Johan Richard, Roland Bacon, Jarle Brinchmann, Thierry Contini, Leclercq, F, Bacon, R, Verhamme, A, Garel, T, Blaizot, J, Brinchmann, J, Cantalupo, S, Claeyssens, A, Conseil, S, Contini, T, Hashimoto, T, Herenz, E, Kusakabe, H, Marino, R, Maseda, M, Matthee, J, Mitchell, P, Pezzuli, G, Richard, J, Schmidt, K, Wisotzki, L, 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), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)

Subjects
Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Scattering, Galaxies: high-redshift, Galaxies: evolution, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxies: formation, Hubble Ultra-Deep Field, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Cosmology: observation, Redshift, Galaxy, Full width at half maximum, Wavelength, Space and Planetary Science, 0103 physical sciences, Radiative transfer, Halo, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We present spatially resolved maps of six individually-detected Lyman alpha haloes (LAHs) as well as a first statistical analysis of the Lyman alpha (Lya) spectral signature in the circum-galactic medium of high-redshift star-forming galaxies using MUSE. Our resolved spectroscopic analysis of the LAHs reveals significant intrahalo variations of the Lya line profile. Using a three-dimensional two-component model for the Lya emission, we measure the full width at half maximum (FWHM), the peak velocity shift and the asymmetry of the Lya line in the core and in the halo of 19 galaxies. We find that the Lya line shape is statistically different in the halo compared to the core for ~40% of our galaxies. Similarly to object-by-object based studies and a recent resolved study using lensing, we find a correlation between the peak velocity shift and the width of the Lya line both at the interstellar and circum-galactic scales. While there is a lack of correlation between the spectral properties and the spatial scale lengths of our LAHs, we find a correlation between the width of the line in the LAH and the halo flux fraction. Interestingly, UV bright galaxies show broader, more redshifted and less asymmetric Lya lines in their haloes. The most significant correlation found is for the FWHM of the line and the UV continuum slope of the galaxy, suggesting that the redder galaxies have broader Lya lines. The generally broad and red line shapes found in the halo component suggests that the Lya haloes are powered either by scattering processes through an outflowing medium, fluorescent emission from outflowing cold clumps of gas, or a mix of both. Considering the large diversity of the Lya line profiles observed in our sample and the lack of strong correlation, the interpretation of our results is still broadly open and underlines the need for realistic spatially resolved models of the LAHs., Comment: 17+4 pages, 12+3 figures, 2+1 tables, accepted for publication in A&A

Published
2020
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8. Nearly all the sky is covered by Lyman-alpha emission around high redshift galaxies

Author

S. Cantalupo, Peter M. Weilbacher, Philipp Richter, R. Saust, J. Kerutt, Jarle Brinchmann, Floriane Leclercq, Lutz Wisotzki, Johan Richard, E. C. Herenz, Tanya Urrutia, T. Contini, Mohammad Akhlaghi, Nicolas Bouché, Matthias Steinmetz, Themiya Nanayakkara, Raffaella Anna Marino, Joop Schaye, Hanae Inami, A. Monreal-Ibero, Martin Wendt, Kasper B. Schmidt, B. Guiderdoni, Roland Bacon, Michael V. Maseda, Wisotzki, L, Bacon, R, Brinchmann, J, Cantalupo, S, Richter, P, Schaye, J, Schmidt, K, Urrutia, T, Weilbacher, P, Akhlaghi, M, Bouche, N, Contini, T, Guiderdoni, B, Herenz, E, Inami, H, Kerutt, J, Leclercq, F, Marino, R, Maseda, M, Monreal-Ibero, A, Nanayakkara, T, Richard, J, Saust, R, Steinmetz, M, and Wendt, M

Subjects
media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Spectral line, 0103 physical sciences, ddc:530, Surface brightness, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Physics, Very Large Telescope, Multidisciplinary, Line-of-sight, 010308 nuclear & particles physics, galaxie, Institut für Physik und Astronomie, Quasar, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, 3. Good health, Cosmology, Galaxies and clusters, 13. Climate action, Sky, Astrophysics of Galaxies (astro-ph.GA)
Abstract

Galaxies are surrounded by large reservoirs of gas, mostly hydrogen, fed by inflows from the intergalactic medium and by outflows due to galactic winds. Absorption-line measurements along the sightlines to bright and rare background quasars indicate that this circumgalactic medium pervades far beyond the extent of starlight in galaxies, but very little is known about the spatial distribution of this gas. A new window into circumgalactic environments was recently opened with the discovery of ubiquitous extended Lyman-alpha emission from hydrogen around high-redshift galaxies, facilitated by the extraordinary sensitivity of the MUSE instrument at the ESO Very Large Telescope. Due to the faintness of this emission, such measurements were previously limited to especially favourable systems or to massive statistical averaging. Here we demonstrate that low surface brightness Lyman-alpha emission surrounding faint galaxies at redshifts between 3 and 6 adds up to a projected sky coverage of nearly 100%. The corresponding rate of incidence (the mean number of Lyman-alpha emitters penetrated by any arbitrary line of sight) is well above unity and similar to the incidence rate of high column density absorbers frequently detected in the spectra of distant quasars. This similarity suggests that most circumgalactic atomic hydrogen at these redshifts has now been detected also in emission., published in Nature, online on 01 Oct 2018, in print on 11 Oct 2018. This is the Authors' version, for the published version see https://www.nature.com/articles/s41586-018-0564-6 ; free viewing access via https://rdcu.be/8eCx

Published
2018

9. Recovering the systemic redshift of galaxies from their Lyman alpha line profile

Author

Sebastiano Cantalupo, Nicolas Bouché, Roland Bacon, Floriane Leclercq, Thierry Contini, Johan Richard, Anne Verhamme, Edmund Christian Herenz, Kasper B. Schmidt, B. Clement, Wolfram Kollatschny, Joseph Caruana, Hanae Inami, Johannes Zabl, C. Diener, Lutz Wisotzki, Joop Schaye, Jarle Brinchmann, Michael V. Maseda, Alyssa B. Drake, Vera Patrício, E. Ventou, Takuya Hashimoto, J. Kerutt, Thibault Garel, R. A. Marino, 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 Physique Théorique - UMR CNRS 3681 (IPHT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-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), Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), 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), Verhamme, A, Garel, T, Ventou, E, Contini, T, Bouche, N, Herenz, E, Richard, J, Bacon, R, Schmidt, K, Maseda, M, Marino, R, Brinchmann, J, Cantalupo, S, Caruana, J, Clement, B, Diener, C, Drake, A, Hashimoto, T, Inami, H, Kerutt, J, Kollatschny, W, Leclercq, F, Patricio, V, Schaye, J, Wisotzki, L, and Zabl, J

Subjects
Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, FOS: Physical sciences, galaxies: starburst, Astronomy and Astrophysics, Lyman-alpha line, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Redshift, Galaxy, Spectral line, galaxies: high-redshift, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, galaxies: statistic, ultraviolet: galaxies, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Line (formation)
Abstract

The Lyman alpha (lya) line of Hydrogen is a prominent feature in the spectra of star-forming galaxies, usually redshifted by a few hundreds of km/s compared to the systemic redshift. This large offset hampers follow-up surveys, galaxy pair statistics and correlations with quasar absorption lines when only lya is available. We propose diagnostics that can be used to recover the systemic redshift directly from the properties of the lya line profile. We use spectroscopic observations of Lyman-Alpha Emitters (LAEs) for which a precise measurement of the systemic redshift is available. Our sample contains 13 sources detected between z~3 and z~6 as part of various Multi Unit Spectroscopic Explorer (MUSE) Guaranteed Time Observations (GTO). We also include a compilation of spectroscopic lya data from the literature spanning a wide redshift range (z~0-8). First, restricting our analysis to double-peaked lya spectra, we find a tight correlation between the velocity offset of the red peak with respect to the systemic redshift, Vpeak, and the separation of the peaks. Secondly, we find a correlation between Vpeak and the full width at half maximum of the lya line. Fitting formulas, to estimate systemic redshifts of galaxies with an accuracy of +-100 km/s when only the lya emission line is available, are given for the two methods., Comment: letter, accepted for publication in MNRAS

Published
2018
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10. Dark Galaxy Candidates at Redshift ∼3.5 Detected with MUSE

Author

C. Diener, Roland Bacon, Lorrie A. Straka, Joseph Caruana, Jarle Brinchmann, Raffaella Anna Marino, Thierry Contini, Sofia G. Gallego, Lutz Wisotzki, H. Finley, Elena Borisova, Simon J. Lilly, Joop Schaye, Martin Wendt, Floriane Leclercq, Johan Richard, Simon Conseil, Hanae Inami, Gabriele Pezzulli, Sowgat Muzahid, Sebastiano Cantalupo, C. Marcella Carollo, Anna Marino, R, Cantalupo, S, Lilly, S, Gallego, S, Straka, L, Borisova, E, Pezzulli, G, Bacon, R, Brinchmann, J, Carollo, C, Caruana, J, Conseil, S, Contini, T, Diener, C, Finley, H, Inami, H, Leclercq, F, Muzahid, S, Richard, J, Schaye, J, Wendt, M, Wisotzki, L, Department of Computer Science [ETH Zürich] (D-INFK), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), 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), 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
FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 010305 fluids & plasmas, Red shift -- Observations, galaxies: high-redshift, quasars: general, 0103 physical sciences, Galaxy formation and evolution, galaxies: formation, Cosmology -- Observations, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Galaxies -- Observations, Galaxies -- Formation, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Star formation, Astronomy and Astrophysics, Quasar, Galaxies, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Cosmology, Stars, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Galaxies -- Evolution, galaxies: star formation, Dark galaxy, intergalactic medium, Equivalent width, quasars: emission line
Abstract

Recent theoretical models suggest that the early phase of galaxy formation could involve an epoch when galaxies are gas-rich but inefficient at forming stars: a "dark galaxy" phase. Here, we report the results of our MUSE (Multi Unit Spectroscopic Explorer) survey for dark galaxies fluorescently illuminated by quasars at $z>3$. Compared to previous studies which are based on deep narrow-band (NB) imaging, our integral field survey provides a nearly uniform sensitivity coverage over a large volume in redshift space around the quasars as well as full spectral information at each location. Thanks to these unique features, we are able to build control samples at large redshift distances from the quasars using the same data taken under the same conditions. By comparing the rest-frame equivalent width (EW$_{0}$) distributions of the Ly$\alpha$ sources detected in proximity to the quasars and in control samples, we detect a clear correlation between the locations of high EW$_{0}$ objects and the quasars. This correlation is not seen in other properties such as Ly$\alpha$ luminosities or volume overdensities, suggesting the possible fluorescent nature of at least some of these objects. Among these, we find 6 sources without continuum counterparts and EW$_{0}$ limits larger than $240\,\mathrm{\AA}$ that are the best candidates for dark galaxies in our survey at $z>3.5$. The volume densities and properties, including inferred gas masses and star formation efficiencies, of these dark galaxy candidates are similar to previously detected candidates at $z\approx2.4$ in NB surveys. Moreover, if the most distant of these are fluorescently illuminated by the quasar, our results also provide a lower limit of $t=60$ Myr on the quasar lifetime., Comment: 28 pages, 13 figures, 5 tables, submitted to ApJ

Published
2018
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11. The MUSE Hubble Ultra Deep Field Survey

Author

Jeremy Blaizot, Mohammad Akhlaghi, Peter D. Mitchell, Hanae Inami, Simon Conseil, Roland Bacon, Sebastiano Cantalupo, Marcella Carollo, Floriane Leclercq, Johan Richard, Anne Verhamme, Joop Schaye, Jarle Brinchmann, Raffaella Anna Marino, Michael V. Maseda, Thierry Contini, Edmund Christian Herenz, Lutz Wisotzki, Takuya Hashimoto, Thibault Garel, 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 Physique Théorique - UMR CNRS 3681 (IPHT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-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), Institut de Chimie de Strasbourg, Université de Strasbourg (UNISTRA)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Leclercq, F, Bacon, R, Wisotzki, L, Mitchell, P, Garel, T, Verhamme, A, Blaizot, J, Hashimoto, T, Herenz, E, Conseil, S, Cantalupo, S, Inami, H, Contini, T, Richard, J, Maseda, M, Schaye, J, Marino, R, Akhlaghi, M, Brinchmann, J, Carollo, M, École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), 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), and Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC)

Subjects
Physics, 010308 nuclear & particles physics, Continuum (design consultancy), Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Hubble Ultra-Deep Field, 01 natural sciences, Cosmology: observation, Galaxy, Redshift, Accretion (astrophysics), Dark matter halo, 13. Climate action, Space and Planetary Science, galaxies: high-redshift, cosmology: observations, 0103 physical sciences, Satellite galaxy, galaxies: formation, Halo, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We report the detection of extended Lyα haloes around 145 individual star-forming galaxies at redshifts 3 ≤ z ≤ 6 in the Hubble Ultra Deep Field observed with the Multi-Unit Spectroscopic Explorer (MUSE) at ESO-VLT. Our sample consists of continuum-faint (− 15 ≥ MUV ≥ −22) Lyα emitters (LAEs). Using a 2D, two-component (continuum-like and halo) decomposition of Lyα emission assuming circular exponential distributions, we measure scale lengths and luminosities of Lyα haloes. We find that 80% of our objects having reliable Lyα halo measurements show Lyα emission that is significantly more extended than the UV continuum detected by HST (by a factor ≈4 to >20). The median exponential scale length of the Lyα haloes in our sample is ≈4.5 kpc with a few haloes exceeding 10 kpc. By comparing the maximal detected extent of the Lyα emission with the predicted dark matter halo virial radii of simulated galaxies, we show that the detected Lyα emission of our selected sample of Lyα emitters probes a significant portion of the cold circum-galactic medium of these galaxies (>50% in average). This result therefore shows that there must be significant HI reservoirs in the circum-galactic medium and reinforces the idea that Lyα haloes are ubiquitous around high-redshift Lyα emitting galaxies. Our characterization of the Lyα haloes indicates that the majority of the Lyα flux comes from the halo (≈65%) and that their scale lengths seem to be linked to the UV properties of the galaxies (sizes and magnitudes). We do not observe a significant Lyα halo size evolution with redshift, although our sample for z> 5 is very small. We also explore the diversity of the Lyα line profiles in our sample and we find that the Lyα lines cover a large range of full width at half maximum (FWHM) from 118 to 512 km s-1. While the FWHM does not seem to be correlated to the Lyα scale length, most compact Lyα haloes and those that are not detected with high significance tend to have narrower Lyα profiles (-1). Finally, we investigate the origin of the extended Lyα emission but we conclude that our data do not allow us to disentangle the possible processes, i.e. scattering from star-forming regions, fluorescence, cooling radiation from cold gas accretion, and emission from satellite galaxies.

Published
2017
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12. Strong lensing analysis of Abell 2744 with MUSE and Hubble Frontier Fields images

Author

Guillaume Mahler, Vera Patrício, Marcella Carollo, Roland Bacon, Lutz Wisotzki, B. Clement, G. Soucail, Rychard Bouwens, Floriane Leclercq, J. Martinez, Johan Richard, D. Lagattuta, Michael V. Maseda, R. Pello, Hanae Inami, Kasper B. Schmidt, 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
galaxies: high redshift, Dark matter, Continuum (design consultancy), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, dark matter, Data cube, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Cluster (physics), 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Remote sensing, Line (formation), Physics, 010308 nuclear & particles physics, galaxies: clusters: individual: Abell 2744, gravitational lensing: strong, Astronomy and Astrophysics, Image plane, Astrophysics - Astrophysics of Galaxies, Redshift, Abell 2744, Space and Planetary Science, techniques: imaging spectroscopy, Astrophysics of Galaxies (astro-ph.GA)
Abstract

We present an analysis of MUSE observations obtained on the massive Frontier Fields cluster Abell 2744. This new dataset covers the entire multiply-imaged region around the cluster core. We measure spectroscopic redshifts for HST-selected continuum sources together with line emitters blindly detected in the datacube. The combined catalog consists of 514 spectroscopic redshifts (with 414 new identifications), including 156 cluster members and 326 magnified background sources. We use this redshift information to perform a strong-lensing analysis of all multiple images previously found in the deep Frontier Field images, and add three new MUSE-detected multiply-imaged systems with no obvious HST counterpart. The combined strong lensing constraints include a total of 60 systems producing 188 images altogether, out of which 29 systems and 83 images are spectroscopically confirmed, making Abell 2744 one of the most well-constrained clusters to date. A parametric mass model including two cluster-scale components in the core and several group-scale substructures at larger radii accurately reproduces all the spectroscopic multiple systems, reaching an rms of 0.67" in the image plane. Overall, the large number of spectroscopic redshifts gives us a robust model and we estimate the systematics on the mass density and magnification within the cluster core to be typically ~9%., 34 pages, 20 figures. Accepted for publication in MNRAS. Full high resolution pdf and other data are available at http://muse-vlt.eu/science/a2744/

Published
2017
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13. The MUSE Hubble Ultra Deep Field Survey. II. Spectroscopic redshifts and comparisons to color selections of high-redshift galaxies

Author

Simon Conseil, Lutz Wisotzki, Joop Schaye, E. Ventou, Jarle Brinchmann, Michael V. Maseda, Alyssa B. Drake, Stephen Hamer, Nicolas Bouché, Laurence Tresse, Hanae Inami, Roland Bacon, Raffaella Anna Marino, Wolfram Kollatschny, H. Finley, Léo Michel-Dansac, Leindert Boogaard, Benjamin Clément, G. Desprez, Thierry Contini, Mieke Paalvast, Floriane Leclercq, Johan Richard, Takuya Hashimoto, Mohammad Akhlaghi, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - 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), Centre Hospitalier Universitaire [Rennes], Nutrition, Métabolismes et Cancer (NuMeCan), Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES), 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), 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), Institut National de la Recherche Agronomique (INRA)-Université de Rennes (UR)-Institut National de la Santé et de la Recherche Médicale (INSERM), Centre National de la Recherche Scientifique (CNRS)-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)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), Équipe de droit international, européen et comparé (EDIEC), Université Jean Moulin - Lyon 3 (UJML), and Université de Lyon-Université de Lyon

Subjects
astro-ph.GA, Continuum (design consultancy), Flux, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, surveys, galaxies: high-redshift, 0103 physical sciences, galaxies: formation, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Line (formation), Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Hubble Ultra-Deep Field, Multi Unit Spectroscopic Explorer, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Magnitude (astronomy), galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], catalogs
Abstract

We have conducted a two-layered spectroscopic survey (1'x1' ultra deep and 3'x3' deep regions) in the Hubble Ultra Deep Field (HUDF) with the Multi Unit Spectroscopic Explorer (MUSE). The combination of a large field of view, high sensitivity, and wide wavelength coverage provides an order of magnitude improvement in spectroscopically confirmed redshifts in the HUDF; i.e., 1206 secure spectroscopic redshifts for HST continuum selected objects, which corresponds to 15% of the total (7904). The redshift distribution extends well beyond z>3 and to HST/F775W magnitudes as faint as ~30 mag (AB, 1-sigma). In addition, 132 secure redshifts were obtained for sources with no HST counterparts that were discovered in the MUSE data cubes by a blind search for emission-line features. In total, we present 1338 high quality redshifts, which is a factor of eight increase compared with the previously known spectroscopic redshifts in the same field. We assessed redshifts mainly with the spectral features [OII] at z~20% up to 28-29 mag and ~27 mag, respectively. We used the determined redshifts to test continuum color selection (dropout) diagrams of high-z galaxies. The selection condition for F336W dropouts successfully captures ~80% of the targeted z~2.7 galaxies. However, for higher redshift selections (F435W, F606W, and F775W dropouts), the success rates decrease to ~20-40%. We empirically redefine the selection boundaries to make an attempt to improve them to ~60%. The revised boundaries allow bluer colors that capture Lya emitters with high Lya equivalent widths falling in the broadbands used for the color-color selection. Along with this paper, we release the redshift and line flux catalog., Comment: 26 pages, 26 figures, 4 tables, accepted for publication in A&A (MUSE UDF Series Paper II), the redshift catalogs will be available at the CDS

Published
2017
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14. The MUSE Hubble Ultra Deep Field Survey VI: The Faint-End of the Ly$\alpha$ Luminosity Function at $2.91 < z < 6.64$ and Implications for Reionisation

Author

R. Pello, Lutz Wisotzki, Simon Conseil, Raffaella Anna Marino, Peter M. Weilbacher, Jeremy Blaizot, Hanae Inami, Takuya Hashimoto, Thierry Contini, Guillaume Mahler, Roland Bacon, E. Ventou, J. Lewis, Joseph Caruana, Floriane Leclercq, Thibault Garel, Johan Richard, Edmund Christian Herenz, Anne Verhamme, Alyssa B. Drake, B. Guiderdoni, Joop Schaye, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS 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 Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), 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), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), 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), Centre de Recherche Astrophysique de Lyon ( CRAL ), École normale supérieure - Lyon ( ENS 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 ), and Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS )

Subjects
[ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, first stars, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Parameter space, 01 natural sciences, 0103 physical sciences, galaxies: formation, dark ages, 010303 astronomy & astrophysics, Reionization, Astrophysics::Galaxy Astrophysics, Physics, COSMIC cancer database, 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, early Universe, Hubble Ultra-Deep Field, Redshift, Galaxy, galaxies: luminosity function, Space and Planetary Science, mass function, Dark Ages, reionization, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the deepest study to date of the Lya luminosity function (LF) in a blank field using blind integral field spectroscopy from MUSE. We constructed a sample of 604 Lya emitters (LAEs) across the redshift range 2.91 < z < 6.64 using automatic detection software in the Hubble Ultra Deep Field. We calculate accurate total Lya fluxes capturing low surface brightness extended Lya emission now known to be a generic property of high-redshift star-forming galaxies. We simulated realistic extended LAEs to characterise the selection function of our samples, and performed flux-recovery experiments to test and correct for bias in our determination of total Lya fluxes. We find an accurate completeness correction accounting for extended emission reveals a very steep faint-end slope of the LF, alpha, down to luminosities of log10 L erg s^-1< 41.5, applying both the 1/Vmax and maximum likelihood estimators. Splitting the sample into three broad redshift bins, we see the faint-end slope increasing from -2.03+1.42-inf at z ~ 3.44 to -2.86+0.76-inf at z ~ 5.48, however no strong evolution is seen between the 68% confidence regions in L*-alpha parameter space. Using the Lya line flux as a proxy for star formation activity, and integrating the observed LFs, we find that LAEs' contribution to the cosmic SFRD rises with redshift until it is comparable to that from continuum-selected samples by z ~ 6. This implies that LAEs may contribute more to the star-formation activity of the early Universe than previously thought - any additional interglactic medium correction would act to further boost the Lya luminosities. Finally, assuming fiducial values for the escape of Lya and LyC radiation, and the clumpiness of the IGM, we integrated the maximum likelihood LF at 5.00 < z < 6.64 and find we require only a small extrapolation beyond the data (< 1 dex in L) for LAEs alone to maintain an ionised IGM at z ~ 6., Comment: 16 pages, 10 figures. Accepted for publication in A&A special issue: "The MUSE Hubble Ultra Deep Field Survey" (MUSE UDF Series Paper VI)

Published
2017
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15. The MUSEHubbleUltra Deep Field Survey

Author

Alyssa B. Drake, R. J. Bouwens, Edmund Christian Herenz, Raffaella Anna Marino, Marcella Carollo, Joseph Caruana, Jarle Brinchmann, Sebastiano Cantalupo, J. Kerutt, Jeremy Blaizot, Joop Schaye, Peter D. Mitchell, Hanae Inami, Floriane Leclercq, Johan Richard, B. Guiderdoni, Anne Verhamme, Roland Bacon, Thibault Garel, and Takuya Hashimoto

Subjects
Physics, Very Large Telescope, 010308 nuclear & particles physics, Continuum (design consultancy), Astronomy and Astrophysics, Astrophysics, Hubble Ultra-Deep Field, 01 natural sciences, Photometry (optics), 13. Climate action, Space and Planetary Science, 0103 physical sciences, Galaxy formation and evolution, Radiative transfer, Emission spectrum, Spectroscopy, 010303 astronomy & astrophysics
Abstract

We present rest-frame Lyα equivalent widths (E W 0 ) of 417 Lyα emitters (LAEs) detected with Multi Unit Spectroscopic Explorer (MUSE) on the Very Large Telescope (VLT) at 2.9 Ultra Deep Field. Based on the deep MUSE spectroscopy and ancillary Hubble Space Telescope (HST) photometry data, we carefully measured E W 0 values taking into account extended Lyα emission and UV continuum slopes (β ). Our LAEs reach unprecedented depths, both in Lyα luminosities and UV absolute magnitudes, from log (L Lyα /erg s-1 ) ~ 41.0 to 43.0 and from M UV ~ −16 to −21 (0.01−1.0 L * z =3 ). The E W 0 values span the range of ~ 5 to 240 A or larger, and their distribution can be well fitted by an exponential law N = N 0 exp(−E W 0 /w 0 ). Owing to the high dynamic range in M UV , we find that the scale factor, w 0 , depends on M UV in the sense that including fainter M UV objects increases w 0 , i.e., the Ando effect. The results indicate that selection functions affect the E W 0 scale factor. Taking these effects into account, we find that our w 0 values are consistent with those in the literature within 1σ uncertainties at 2.9 UV and L Lyα . Interestingly, we find 12 objects with E W 0 > 200 A above 1σ uncertainties. Two of these 12 LAEs show signatures of merger or AGN activity: the weak Civλ 1549 emission line. For the remaining 10 very large E W 0 LAEs, we find that the E W 0 values can be reproduced by young stellar ages ( ⊙ ). Otherwise, at least part of the Lyα emission in these LAEs needs to arise from anisotropic radiative transfer effects, fluorescence by hidden AGN or quasi-stellar object activity, or gravitational cooling.

Published
2017
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