Publication

Microlensing flux ratio predictions for Euclid

Vernardos, G., Mar-2019, In : Monthly Notices of the Royal Astronomical Society. 483, 4, p. 5583-5594 12 p.

Research output: Contribution to journalArticleAcademicpeer-review

APA

Vernardos, G. (2019). Microlensing flux ratio predictions for Euclid. Monthly Notices of the Royal Astronomical Society, 483(4), 5583-5594. https://doi.org/10.1093/mnras/sty3486

Author

Vernardos, G. / Microlensing flux ratio predictions for Euclid. In: Monthly Notices of the Royal Astronomical Society. 2019 ; Vol. 483, No. 4. pp. 5583-5594.

Harvard

Vernardos, G 2019, 'Microlensing flux ratio predictions for Euclid', Monthly Notices of the Royal Astronomical Society, vol. 483, no. 4, pp. 5583-5594. https://doi.org/10.1093/mnras/sty3486

Standard

Microlensing flux ratio predictions for Euclid. / Vernardos, G.

In: Monthly Notices of the Royal Astronomical Society, Vol. 483, No. 4, 03.2019, p. 5583-5594.

Research output: Contribution to journalArticleAcademicpeer-review

Vancouver

Vernardos G. Microlensing flux ratio predictions for Euclid. Monthly Notices of the Royal Astronomical Society. 2019 Mar;483(4):5583-5594. https://doi.org/10.1093/mnras/sty3486


BibTeX

@article{64f7513e34624a7ea22db82fb3961d73,
title = "Microlensing flux ratio predictions for Euclid",
abstract = "Quasar microlensing flux ratios are used to unveil properties of the lenses in large collections of lensed quasars, like the ones expected to be produced by the Euclid survey. This is achieved using the direct survey products, without any (expensive) follow-up observations or monitoring. First, the theoretical flux ratio distribution of samples of hundreds of mock quasar lenses is calculated for different initial mass functions (IMFs) and Sersic radial profiles for the lens compact matter distribution. Then, mock observations are created and compared to the models to recover the underlying one. The most important factor for determining the flux ratio properties of such samples is the value of the smooth matter fraction at the location of the multiple images. Doubly lensed CASTLES-like quasars are the most promising systems to constrain the IMF and the mass components for a sample of lenses.",
keywords = "gravitational lensing: micro, galaxies: stellar content, DARK-MATTER SUBSTRUCTURE, ACCRETION DISC, MASS, STELLAR, MAGNIFICATION, PROFILES, GALAXIES",
author = "G. Vernardos",
year = "2019",
month = "3",
doi = "10.1093/mnras/sty3486",
language = "English",
volume = "483",
pages = "5583--5594",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "4",

}

RIS

TY - JOUR

T1 - Microlensing flux ratio predictions for Euclid

AU - Vernardos, G.

PY - 2019/3

Y1 - 2019/3

N2 - Quasar microlensing flux ratios are used to unveil properties of the lenses in large collections of lensed quasars, like the ones expected to be produced by the Euclid survey. This is achieved using the direct survey products, without any (expensive) follow-up observations or monitoring. First, the theoretical flux ratio distribution of samples of hundreds of mock quasar lenses is calculated for different initial mass functions (IMFs) and Sersic radial profiles for the lens compact matter distribution. Then, mock observations are created and compared to the models to recover the underlying one. The most important factor for determining the flux ratio properties of such samples is the value of the smooth matter fraction at the location of the multiple images. Doubly lensed CASTLES-like quasars are the most promising systems to constrain the IMF and the mass components for a sample of lenses.

AB - Quasar microlensing flux ratios are used to unveil properties of the lenses in large collections of lensed quasars, like the ones expected to be produced by the Euclid survey. This is achieved using the direct survey products, without any (expensive) follow-up observations or monitoring. First, the theoretical flux ratio distribution of samples of hundreds of mock quasar lenses is calculated for different initial mass functions (IMFs) and Sersic radial profiles for the lens compact matter distribution. Then, mock observations are created and compared to the models to recover the underlying one. The most important factor for determining the flux ratio properties of such samples is the value of the smooth matter fraction at the location of the multiple images. Doubly lensed CASTLES-like quasars are the most promising systems to constrain the IMF and the mass components for a sample of lenses.

KW - gravitational lensing: micro

KW - galaxies: stellar content

KW - DARK-MATTER SUBSTRUCTURE

KW - ACCRETION DISC

KW - MASS

KW - STELLAR

KW - MAGNIFICATION

KW - PROFILES

KW - GALAXIES

U2 - 10.1093/mnras/sty3486

DO - 10.1093/mnras/sty3486

M3 - Article

VL - 483

SP - 5583

EP - 5594

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 4

ER -

ID: 107819770