The MUSE<i>Hubble</i>Ultra Deep Field Survey

Ventou, E.; Contini, T.; Bouché, Nicolas; Épinat, B.; Brinchmann, Jarle; Bacon, Roland; Inami, Hanae; Lam, Daniel; Drake, Alyssa B.; Garel, Thibault; Michel-Dansac, Léo; Pelló, R.; Steinmetz, Matthias; Weilbacher, Peter M.; Wisotzki, L.; Carollo, M.

doi:10.1051/0004-6361/201731586

Cited by 82 publications

(128 citation statements)

References 95 publications

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“…However, the error for the LAE fraction should be derived by BPCI like in other fraction studies (e.g. the galaxy merger fraction, Ventou et al 2017) to obtain statistically correct errors. The BPCI method is reviewed for astronomical uses in Cameron (2011).…”

Section: Lae and Its Error Budgetmentioning

confidence: 99%

The MUSEHubbleUltra Deep Field Survey

Kusakabe

Blaizot

Garel

et al. 2020

A&A

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Context. The Lyα 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. Aims. Thanks to deep data obtained with the integral field spectrograph MUSE (Multi-Unit Spectroscopic Explorer), we can measure the evolution of the LAE fraction homogeneously over a wide redshift range of z ≈ 3-6 for UV-faint galaxies (down to UV magnitudes of M 1500 ≈ −17.75). This is significantly fainter than in former studies (M 1500 ≤ −18.75), and allows us to probe the bulk of the population of high-redshift star-forming galaxies. Methods. We construct a UV-complete photometric-redshift sample following UV luminosity functions and measure the Lyα emission with MUSE using the latest (second) data release from the MUSE Hubble Ultra Deep Field Survey. Results. We derive the redshift evolution of X LAE for M 1500 ∈ [−21.75; −17.75] for the first time with a equivalent width range EW(Lyα) ≥ 65 Å and find low values of X LAE 30% at z 6. The best fit linear relation is X LAE = 0.07 +0.06 −0.03 z − 0.22 +0.12 −0.24 . For M 1500 ∈ [−20.25; −18.75] and EW(Lyα) ≥ 25 Å, our X LAE values are consistent with those in the literature within 1σ at z 5, but our median values are systematically lower than reported values over the whole redshift range. In addition, we do not find a significant dependence of X LAE on M 1500 for EW(Lyα) ≥ 50 Å 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 Lyα emission, hence X LAE is biased towards higher values when those samples are used. Conclusions. 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 LAE fractions much better than models where SF is a smooth function of time.

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Section: Lae and Its Error Budgetmentioning

confidence: 99%

The MUSEHubbleUltra Deep Field Survey

Kusakabe

Blaizot

Garel

et al. 2020

A&A

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“…We consider only pairs of galaxies with a stellar mass ratio between unity and 1:4 ("major merger") at the present day. Lastly, the majority of observations (e.g., Bridge et al 2010;Ellison et al 2010;Larson et al 2016;Ventou et al 2017;Mantha et al 2018) and idealised simulations (e.g., Toomre & Toomre 1972;Barnes & Hernquist 1991, 1996Di Matteo et al 2008;Lotz et al 2008;Rupke et al 2010;Bournaud et al 2011;Hopkins et al 2013;Moreno et al 2015Moreno et al , 2019 of galaxy mergers typically assume the system is composed of only two galaxies. In order to approximate this assumption, we required that any tertiary subhalo in the FoF group be at most 1/16 the stellar mass of the primary (or, most massive) halo.…”

Section: Parent Samplementioning

confidence: 99%

Galaxy interactions in IllustrisTNG-100, I: The power and limitations of visual identification

Blumenthal

Moreno

Barnes

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present a sample of 446 galaxy pairs constructed using the cosmological simulation IllustrisTNG-100 at z = 0, with M FoF, dm = 10 11 − 10 13.5 M . We produce ideal mock SDSS g-band images of all pairs to test the reliability of visual classification schema employed to produce samples of interacting galaxies. We visually classify each image as interacting or not based on the presence of a close neighbour, the presence of stellar debris fields, disturbed discs, and/or tidal features. By inspecting the trajectories of the pairs, we determine that these indicators correctly identify interacting galaxies ∼45% of the time. We subsequently split the sample into the visually identified interacting pairs (VIP; 38 pairs) and those which are interacting but are not visually identified (nonVIP; 47 pairs). We find that VIP have undergone a close passage nearly twice as recently as the nonVIP, and typically have higher stellar masses.Further, the VIP sit in dark matter haloes that are approximately 2.5 times as massive, in environments nearly 2 times as dense, and are almost a factor of 10 more affected by the tidal forces of their surroundings than the nonVIP. These factors conspire to increase the observability of tidal features and disturbed morphologies, making the VIP more likely to be identified. Thus, merger rate calculations which rely on stellar morphologies are likely to be significantly biased toward massive galaxy pairs which have recently undergone a close passage.

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“…Extended Lyα haloes around individual Lyα emitters are discussed in Paper VIII (Leclercq et al 2017). The first measurement of the evolution of galaxy merger fraction up to z ≈ 6 is presented in Paper IX (Ventou et al 2017) and a detailed study of Lyα equivalent widths properties of the Lyα emitters is discussed in Paper X (Hashimoto et al 2017).…”

Section: Introductionmentioning

confidence: 99%

The MUSE Hubble Ultra Deep Field Survey

Bacon

Conseil

Mary

et al. 2017

A&A

335

397

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We present the MUSE Hubble Ultra Deep Survey, a mosaic of nine MUSE fields covering 90% of the entire HUDF region with a 10-h deep exposure time, plus a deeper 31-h exposure in a single 1.15 arcmin 2 field. The improved observing strategy and advanced data reduction results in datacubes with sub-arcsecond spatial resolution (0 . 65 at 7000 Å) and accurate astrometry (0 . 07 rms). We compare the broadband photometric properties of the datacubes to HST photometry, finding a good agreement in zeropoint up to m AB = 28 but with an increasing scatter for faint objects. We have investigated the noise properties and developed an empirical way to account for the impact of the correlation introduced by the 3D drizzle interpolation. The achieved 3σ emission line detection limit for a point source is 1.5 and 3.1 × 10 −19 erg s −1 cm −2 for the single ultra-deep datacube and the mosaic, respectively. We extracted 6288 sources using an optimal extraction scheme that takes the published HST source locations as prior. In parallel, we performed a blind search of emission line galaxies using an original method based on advanced test statistics and filter matching. The blind search results in 1251 emission line galaxy candidates in the mosaic and 306 in the ultradeep datacube, including 72 sources without HST counterparts (m AB > 31). In addition 88 sources missed in the HST catalog but with clear HST counterparts were identified. This data set is the deepest spectroscopic survey ever performed. In just over 100 h of integration time, it provides nearly an order of magnitude more spectroscopic redshifts compared to the data that has been accumulated on the UDF over the past decade. The depth and high quality of these datacubes enables new and detailed studies of the physical properties of the galaxy population and their environments over a large redshift range.

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The MUSEHubbleUltra Deep Field Survey

Cited by 82 publications

References 95 publications

The MUSEHubbleUltra Deep Field Survey

The MUSEHubbleUltra Deep Field Survey

Galaxy interactions in IllustrisTNG-100, I: The power and limitations of visual identification

The MUSE Hubble Ultra Deep Field Survey

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