NIP: the near infrared imaging photometer for Euclid

Schweitzer, Mario; Bender, Ralf; Katterloher, R.; Eisenhauer, F.; Hofmann, R.; Saglia, R.; Holmes, Rory; Krause, O.; Rix, Hans─Walter; Booth, Jeff; Fagrelius, Parker; Rhodes, Jason; Seshadri, S. R.; Réfrégier, Alexandre; Amiaux, J.; Auguères, J.-L.; Boulade, O.; Cara, C.; Amara, Adam; Lilly, Simon; Atad-Ettedgui, Eli; Giorgio, A. Di; Duvet, L.; Kuehl, Christopher J.; Syed, Mohsin Ali Shah

doi:10.1117/12.857031

Cited by 5 publications

(3 citation statements)

References 8 publications

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“…We study the performance of the high-resolution visible imager, the more suitable to detailed gravitational lensing work, with the standard survey parameters. The instrument properties are taken from Schweitzer et al 2010 [41], Penny et al 2013 [42] and Cropper et al 2014 [43]. Since the PSF is proprietary to the Euclid team, we adopt for simplicity a Gaussian function with full width half maximum 0.…”

Section: Jcap09(2015)059mentioning

confidence: 99%

Precision cosmology with time delay lenses: high resolution imaging requirements

Meng

Treu

Agnello

et al. 2015

J. Cosmol. Astropart. Phys.

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Abstract. Lens time delays are a powerful probe of cosmology, provided that the gravitational potential of the main deflector can be modeled with sufficient precision. Recent work has shown that this can be achieved by detailed modeling of the host galaxies of lensed quasars, which appear as "Einstein Rings" in high resolution images. The distortion of these arcs and counter-arcs, as measured over a large number of pixels, provides tight constraints on the difference between the gravitational potential between the quasar image positions, and thus on cosmology in combination with the measured time delay. We carry out a systematic exploration of the high resolution imaging required to exploit the thousands of lensed quasars that will be discovered by current and upcoming surveys with the next decade. Specifically, we simulate realistic lens systems as imaged by the Hubble Space Telescope (HST), James Webb Space Telescope (JWST), and ground based adaptive optics images taken with Keck or the Thirty Meter Telescope (TMT). We compare the performance of these pointed observations with that of images taken by the Euclid (VIS), Wide-Field Infrared Survey Telescope (WFIRST) and Large Synoptic Survey Telescope (LSST) surveys. We use as our metric the precision with which the slope γ of the total mass density profile ρ tot ∝ r −γ for the main deflector can be measured. Ideally, we require that the statistical error on γ be less than 0.02, such that it is subdominant to other sources of random and systematic uncertainties. We find that survey data will likely have sufficient depth and resolution to meet the target only for the brighter gravitational lens systems, comparable to those discovered by the SDSS survey. For fainter systems, that will be discovered by current and future surveys, targeted follow-up will be required. However, the exposure time required with upcoming facilitites such as JWST, the Keck Next Generation Adaptive Optics System, and TMT, will only be of order a few minutes per system, thus making the follow-up of hundreds of systems a practical and efficient cosmological probe.arXiv:1506.07640v2 [astro-ph.CO] 1 Sep 2015

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Section: Jcap09(2015)059mentioning

confidence: 99%

Precision cosmology with time delay lenses: high resolution imaging requirements

Meng

Treu

Agnello

et al. 2015

J. Cosmol. Astropart. Phys.

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“…These latter experiments are nonetheless only pathfinders for the unprecedented amount of data and scientific information that will be collected by the Square Kilometre Array Observatory (SKAO, Blyth et al 2015) in the same wavelength range. In a complementary way, the Euclid mission (Amendola et al 2018) with its visible imager (VIS, Cropper et al 2016) and near infrared imaging photometer (NIP, Schweitzer et al 2010), along with the Vera C. Rubin Observatory and its Legacy Survey of Space and Time (LSST, LSST Science Collaboration 2009), as well as the Dark Energy Spectroscopic Instrument (DESI, DESI Collaboration 2016), will probe the visible and infra-red regions of the spectrum on extremely wide areas and high sensitivities.…”

Section: Introductionmentioning

confidence: 99%

GalaPy: A highly optimised C₊₊/Python spectral modelling tool for galaxies

Ronconi,

Lapi,

Torsello

et al. 2024

A&A

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Bolstered by upcoming data from new-generation observational campaigns, we are about to enter a new era in the study of how galaxies form and evolve. The unprecedented quantity of data that will be collected from distances that have only marginally been grasped up to now will require analytical tools designed to target the specific physical peculiarities of the observed sources and handle extremely large datasets. One powerful method to investigate the complex astrophysical processes that govern the properties of galaxies is to model their observed spectral energy distributions (SEDs) at different stages of evolution and times throughout the history of the Universe. To address these challenges, we have developed a new library for modelling and fitting SEDs of galaxies from the X-ray to the radio band, as well as the evolution of their components and dust attenuation and reradiation. On the physical side incorporates both empirical and physically motivated star formation histories (SFHs), state-of-the-art single stellar population synthesis libraries, a two-component dust model for attenuation, an age-dependent energy conservation algorithm to compute dust reradiation, and additional sources of stellar continuum such as synchrotron, nebular and free-free emission, as well as X-ray radiation from low- and high-mass binary stars. On the computational side implements a hybrid approach that combines the high performance of compiled C++ with the user-friendly flexibility of Python. Also, it exploits an object-oriented design via advanced programming techniques. is the fastest SED-generation tool of its kind, with a peak performance of almost 1000 SEDs per second. The models are generated on the fly without relying on templates, thus minimising memory consumption. It exploits a fully Bayesian parameter space sampling, which allows for the inference of parameter posteriors and thereby facilitates the study of the correlations between the free parameters and the other physical quantities that can be derived from modelling. The application programming interface (API) and functions of are under continuous development, with planned extensions in the near future. In this first work, we introduce the project and showcase the photometric SED fitting tools already available to users. is available on the Python Package Index (PyPI) and comes with extensive online documentation and tutorials.

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“…23 (Cropper et al 2010). The complementary Near Infrared Spectrometer and Photometer (NISP) instrument will cover wavelengths from 900 to 2000 nm with three broad-band filters, i.e., Y , J, and H (see Figure 1), and a low-resolution slitless spectrometer (Schweitzer et al 2010). The Euclid Wide Survey is expected to cover 15 000 deg 2 down to 10σ depth of 24.5 mag in the visible filter and down to a 5σ depth of 24.0 mag at nearinfrared wavelengths.…”

mentioning

confidence: 99%

Euclid: the selection of quiescent and star-forming galaxies using observed colours

Bisigello

Kuchner

Conselice

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The Euclid mission will observe well over a billion galaxies out to z ∼ 6 and beyond. This will offer an unrivalled opportunity to investigate several key questions for understanding galaxy formation and evolution. The first step for many of these studies will be the selection of a sample of quiescent and star-forming galaxies, as is often done in the literature by using well known colour techniques such as the 'U V J' diagram. However, given the limited number of filters available for the Euclid telescope, the recovery of such rest-frame colours will be challenging. We therefore investigate the use of observed Euclid colours, on their own and together with ground-based uband observations, for selecting quiescent and star-forming galaxies. The most efficient colour combination, among the ones tested in this work, consists of the (u − V IS) and (V IS − J) colours. We find that this combination allows users to select a sample of quiescent galaxies complete to above ∼ 70% and with less than 15% contamination at redshifts in the range 0.75 < z < 1. For galaxies at high-z or without the u-band complementary observations, the (V IS − Y ) and (J − H) colours represent a valid alternative, with > 65% completeness level and contamination below 20% at 1 < z < 2 for finding quiescent galaxies. In comparison, the sample of quiescent galaxies selected with the traditional U V J technique is only ∼ 20% complete at z < 3, when recovering the rest-frame colours using mock Euclid observations. This shows that our new methodology is the most suitable one when only Euclid bands, along with u-band imaging, are available.

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NIP: the near infrared imaging photometer for Euclid

Cited by 5 publications

References 8 publications

Precision cosmology with time delay lenses: high resolution imaging requirements

Precision cosmology with time delay lenses: high resolution imaging requirements

GalaPy: A highly optimised C₊₊/Python spectral modelling tool for galaxies

Euclid: the selection of quiescent and star-forming galaxies using observed colours

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NIP: the near infrared imaging photometer for Euclid

Cited by 5 publications

References 8 publications

Precision cosmology with time delay lenses: high resolution imaging requirements

Precision cosmology with time delay lenses: high resolution imaging requirements

GalaPy: A highly optimised C++/Python spectral modelling tool for galaxies

Euclid: the selection of quiescent and star-forming galaxies using observed colours

Contact Info

Product

Resources

About

GalaPy: A highly optimised C₊₊/Python spectral modelling tool for galaxies