Rising MOONS: an update on the VLT’s next multi-object spectrograph as it begins to grow

Taylor, W. C.; Cirasuolo, M.; Afonso, J.; Carollo, M.; Evans, C. J.; Flores, H.; Maiolino, R.; Paltani, S.; Vanzi, L.; Abreu, Manuel; Amans, Jean-Phillipe; Atkinson, David; Barrett, Joe; Beard, S. M.; Béchet, Celementine; Black, Martin; Boettger, D.; Brierley, Saskia; Buscher, David F.; Cabral, Alexandre; Cochrane, William; Coelho, João M. P.; Colling, Miriam; Conzelmann, Ralf; D’Alessio, F.; Dauvin, Louise; Davidson, George; Drass, H.; Dünner, Rolando; Fairley, Alasdair; Fasola, Giles; Ferruzzi, D.; Fisher, Martin; Flores, Mauricio; Garilli, B.; Gaudemard, Julien; Gonzalez, O. A.; Guinouard, Isabelle; Gutierrez, P.; Hammersley, P. L.; Haigron, R.; Haniff, C.; Hayati, Mahmoud; Ives, Derek; Iwert, Olaf; Laporte, Philippe; Lee, David; Causi, G. Li; Luco, Yerko; Macleod, Alastair; Mainieri, V.; Maire, C.; Melse, Basile-Thierry; Nix, Johannes; Oliva, E.; Oliveira, Antônio César de; Origlia, L.; Parry, Ian; Pedichini, Fernando; Piazzesi, Roberto; Rees, Phil; Reix, Florent; Rodrigues, M.; Rojas, Felipe; Rota, Stefano; Royer, F.; Santos, P.; Schnell, Robin; Shen, Tzu‐Chiang; Sordet, M.; Strachan, Jonathan; Sun, Xiaowei; Tait, Graham; Torres, Miguel Ángel Pérez; Tozzi, Andre; Tulloch, Simon; Navarro, Álvaro Valenzuela; Dran, Lauren Von; Waring, Chris; Watson, Stephen; Woodward, Brian; Yang, Yanbin

doi:10.1117/12.2313403

Cited by 13 publications

(7 citation statements)

References 2 publications

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“…Clearly to make further progress using this technique we will require large spectroscopic surveys from new instruments such as 4MOST (the 4-metre Multi-Object Spectroscopic Telescope; de Jong et al 2019) and MOONS (Multi Object Optical and Nearinfrared Spectrograph; Taylor et al 2018), matched with high quality imaging to enable citizen science/machine learning morphology classifications for as many galaxies as possible. In addition, better methods for measuring gas-phase metallicities will allow us to make the most of existing observations.…”

Section: Discussionmentioning

confidence: 99%

Gas accretion as fuel for residual star formation in Galaxy Zoo elliptical galaxies

Davis

Young

2019

Monthly Notices of the Royal Astronomical Society: Letters

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In this letter we construct a large sample of early-type galaxies with measured gas-phase metallicities from the Sloan Digital Sky Survey and Galaxy Zoo in order to investigate the origin of the gas that fuels their residual star formation. We use this sample to show that star forming elliptical galaxies have a substantially different gas-phase metallicity distribution from spiral galaxies, with ≈7.4% having a very low gas-phase metallicity for their mass. These systems typically have fewer metals in the gas phase than they do in their stellar photospheres, which strongly suggests that the material fuelling their recent star formation was accreted from an external source. We use a chemical evolution model to show that the enrichment timescale for low-metallicity gas is very short, and thus that cosmological accretion and minor mergers are likely to supply the gas in > ∼ 37% of star-forming ETGs, in good agreement with estimates derived from other independent techniques.

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Section: Discussionmentioning

confidence: 99%

Gas accretion as fuel for residual star formation in Galaxy Zoo elliptical galaxies

Davis

Young

2019

Monthly Notices of the Royal Astronomical Society: Letters

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“…In this perspective, we design each calibration sample to be assembled by means of nextgeneration facilities. For instance the spectroscopic survey required for C1 could be carried out in the optical with the 4-metre Multi-Object Spectroscopic Telescope (4MOST, de Jong et al 2019) and up to 1.8 µm with the Multi-Object Optical and Near-infrared Spectrograph (MOONS, Taylor et al 2018). Both spectrographs will start operations in 2020−2022, at the ESO telescopes VISTA and VLT respectively.…”

Section: How To Build the Sfr Calibration Sample?mentioning

confidence: 99%

horizon-AGN virtual observatory – 2. Template-free estimates of galaxy properties from colours

Davidzon

Laigle

Capak

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Using the Horizon-AGN hydrodynamical simulation and self-organising maps (SOMs), we show how to compress the complex, high-dimensional data structure of a simulation into a 2-d grid, which greatly facilitates the analysis of how galaxy observables are connected to intrinsic properties. We first verify the tight correlation between the observed 0.3−5µm broad-band colours of Horizon-AGN galaxies and their high-resolution spectra. The correlation is found to extend to physical properties such as redshift, stellar mass, and star formation rate (SFR). This direct mapping from colour to physical parameter space is shown to work also after including photometric uncertainties that mimic the COSMOS survey. We then label the SOM grid with a simulated calibration sample, and estimate redshift and SFR for COSMOS-like galaxies up to z ∼ 3. In comparison to state-of-the-art techniques based on synthetic templates, our method is comparable in performance but less biased at estimating redshifts, and significantly better at predicting SFRs. In particular our "data-driven" approach, in contrast to model libraries, intrinsically allows for the complexity of galaxy formation and can handle sample biases. We advocate that obtaining the calibration for this method should be one of the goals of next-generation galaxy surveys.

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“…The Multi-object Optical and Near-IR spectrograph (MOONS; [246]) will be installed on the 8 m Very Large Telescope (VLT) of the European Southern Observatory (ESO). MOONS makes use of the full 25 diameter FOV of the VLT, deploying 1001 fibres to obtain high resolution spectra (R ≈ 20, 000) with simultaneous optical and near-IR (0.6−1.8 µm) coverage.…”

Section: Future Directions and Future Facilitiesmentioning

confidence: 99%

Dynamics of young stellar clusters as planet-forming environments

Reiter

Parker

2022

Eur. Phys. J. Plus

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Most stars and thus most planetary systems do not form in isolation. The larger star-forming environment affects protoplanetary disks in multiple ways: Gravitational interactions with other stars truncate disks and alter the architectures of exoplanet systems; external irradiation from nearby high-mass stars truncates disks and shortens their lifetimes; and the remaining gas and dust in the environment affect dynamical evolution (if removed by feedback processes) and provide some shielding for disks from external irradiation. The dynamical evolution of the region regulates when and how long various feedback mechanisms impact protoplanetary disks. Density is a key parameter that regulates the intensity and duration of UV irradiation and the frequency of dynamical encounters. The evolution of larger star-forming complexes may also play an important role by mixing populations. Observations suggest that clusters are not a single-age population but multiple populations with small age differences, which may be key to resolving several timescale issues (i.e., proplyd lifetimes, enrichment). In this review, we consider stellar clusters as the ecosystems in which most stars and therefore most planets form. We review recent observational and theoretical results and highlight upcoming contributions from facilities expected to begin observations in the next 5 years. Looking further ahead, we argue that the next frontier is large-scale surveys of low-mass stars in more distant high-mass star-forming regions. The future of ecosystem studies is bright as faint low-mass stars in more distant high-mass star-forming regions will be routinely observable in the era of extremely large telescopes.

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Rising MOONS: an update on the VLT’s next multi-object spectrograph as it begins to grow

Cited by 13 publications

References 2 publications

Gas accretion as fuel for residual star formation in Galaxy Zoo elliptical galaxies

Gas accretion as fuel for residual star formation in Galaxy Zoo elliptical galaxies

horizon-AGN virtual observatory – 2. Template-free estimates of galaxy properties from colours

Dynamics of young stellar clusters as planet-forming environments

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