The effects of seeing on Sérsic profiles - II. The Moffat PSF

Trujillo, Ignacio; Aguerri, J. A. L.; Cepa, J.; Gutiérrez, Carlos M.

doi:10.1046/j.1365-8711.2001.04937.x

Cited by 191 publications

(162 citation statements)

References 17 publications

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“…Mass Maps Numerous studied have shown that the ability of recovering intrinsic galaxy properties from observed flux distributions depends strongly on the image S/N, resolution and even on the intrinsic properties of the galaxies themselves (Disney 1976;Schweizer 1979;Franx et al 1989;Impey & Bothun 1997;Trujillo et al 2001;Graham et al 2005;Cameron & Driver 2007;Bailin & Harris 2008;Graham & Worley 2008;Maller et al 2009;Carollo et al 2013a;Cibinel et al 2013a). Our mass-based measurements will also be affected by similar limitations.…”

Section: Systematic Uncertainties In the Reconstructedmentioning

confidence: 99%

A PHYSICAL APPROACH TO THE IDENTIFICATION OF HIGH-ZMERGERS: MORPHOLOGICAL CLASSIFICATION IN THE STELLAR MASS DOMAIN

Cibinel

Floc’h

Perret

et al. 2015

ApJ

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At z 1, the distinction between merging and "normal" star-forming galaxies based on single band morphology is often hampered by the presence of large clumps which result in a disturbed, merger-like appearance even in rotationally supported disks. In this paper we discuss how a classification based on canonical, non-parametric structural indices measured on resolved stellar mass maps, rather than on single-band images, reduces the misclassification of clumpy but not merging galaxies. We calibrate the mass-based selection of mergers using the MIRAGE hydrodynamical numerical simulations of isolated and merging galaxies which span a stellar mass range of 10 9.8 -10 10.6 M ⊙ and merger ratios between 1:1-1:6.3. These simulations are processed to reproduce the typical depth and spatial resolution of observed Hubble Ultra Deep Field (HUDF) data. We test our approach on a sample of real z ≃ 2 galaxies with kinematic classification into disks or mergers and on ∼100 galaxies in the HUDF field with photometric/spectroscopic redshift between 1.5 z 3 and M > 10 9.4 M ⊙ . We find that a combination of the asymmetry A MASS and M 20,MASS indices measured on the stellar mass maps can efficiently identify real (major) mergers with 20% contamination from clumpy disks in the merger sample. This mass-based classification cannot be reproduced in star-forming galaxies by H−band measurements alone, which instead result in a contamination from clumpy galaxies that can be as high as 50%. Moreover, we find that the mass-based classification always results in a lower contamination from clumpy galaxies than an H−band classification, regardless of the depth of the imaging used (e.g.,

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Section: Systematic Uncertainties In the Reconstructedmentioning

confidence: 99%

A PHYSICAL APPROACH TO THE IDENTIFICATION OF HIGH-ZMERGERS: MORPHOLOGICAL CLASSIFICATION IN THE STELLAR MASS DOMAIN

Cibinel

Floc’h

Perret

et al. 2015

ApJ

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“…where the radial scale length α and the slope β are free parameters, which can be related to the seeing by the relation FWHM= 2α √ 2 1/β − 1 (see also Trujillo et al 2001). This method has proved to be suitable in our case due to the presence of extended wings in the PSFs.…”

Section: Data From the Ohp Observatorymentioning

confidence: 92%

GHASP: an Hα kinematic survey of spiral galaxies – X. Surface photometry, decompositions and the Tully–Fisher relation in theR_cband

Barbosa

Oliveira

Amram

et al. 2015

Mon. Not. R. Astron. Soc.

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We present R c -band surface photometry for 170 of the 203 galaxies in GHASP, Gassendi H-Alpha survey of SPirals, a sample of late-type galaxies for which high-resolution FabryPerot H maps have previously been obtained. Our data set is constructed by new R c -band observations taken at the Observatoire de Haute-Provence (OHP), supplemented with Sloan Digital Sky Survey (SDSS) archival data, obtained with the purpose of deriving homogeneous photometric profiles and parameters. Our results include R c -band surface brightness profiles for 170 galaxies and ugriz profiles for 108 of these objects. We catalogue several parameters of general interest for further reference, such as total magnitude, effective radius and isophotal parameters -magnitude, position angle, ellipticity and inclination. We also perform a structural decomposition of the surface brightness profiles using a multi-component method in order to separate disks from bulges and bars, and to observe the main scaling relations involving luminosities, sizes and maximum velocities.We determine the R c -band Tully Fisher relation using maximum velocities derived solely from Hα rotation curves for a sample of 80 galaxies, resulting in a slope of −8.1 ± 0.5, zero point of −3.0 ± 1.0 and an estimated intrinsic scatter of 0.28 ± 0.07. We note that, different from the TF-relation in the near-infrared derived for the same sample, no change in the slope of the relation is seen at the low-mass end (for galaxies with V max < 125 km/s). We suggest that this different behaviour of the Tully Fisher relation (with the optical relation being described by a single power-law while the near-infrared by two) may be caused by differences in the stellar mass to light ratio for galaxies with V max < 125 km/s.

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“…However, a Moffat function is a better fit to the seeing, with only 42% EE in the seeing FWHM (e.g. Trujillo et al 2001 3 ). with HARPS and NIRPS, and 0.5-0.95 µm for the NIRPS alone mode.…”

Section: Ngs Magnitudementioning

confidence: 99%

Adaptive optics for high resolution spectroscopy: a direct application with the future NIRPS spectrograph

et al. 2016

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Radial velocity instruments require high spectral resolution and extreme thermo-mecanical stability, even more difficult to achieve in near-infra red (NIR) where the spectrograph has to be cooled down. For a seeing-limited spectrograph, the price of high spectral resolution is an increased instrument volume, proportional to the diameter of the primary mirror. A way to control the size, cost, and stability of radial velocity spectrographs is to reduce the beam optical etendue thanks to an Adaptive Optics (AO) system. While AO has revolutionized the field of high angular resolution and high contrast imaging during the last 20 years, it has not yet been (successfully) used as a way to control spectrographs size, especially in the field of radial velocities.In this work we present the AO module of the future NIRPS spectrograph for the ESO 3.6 m telescope, that will be feed with multi-mode fibers. We converge to an AO system using a Shack-Hartmann wavefront sensor with 14x14 subapertures, able to feed 50% of the energy into a 0.4" fiber in the range of 0.98 to 1.8 µm for M-type stars as faint as I=12.

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The effects of seeing on Sérsic profiles - II. The Moffat PSF

Cited by 191 publications

References 17 publications

A PHYSICAL APPROACH TO THE IDENTIFICATION OF HIGH-ZMERGERS: MORPHOLOGICAL CLASSIFICATION IN THE STELLAR MASS DOMAIN

A PHYSICAL APPROACH TO THE IDENTIFICATION OF HIGH-ZMERGERS: MORPHOLOGICAL CLASSIFICATION IN THE STELLAR MASS DOMAIN

GHASP: an Hα kinematic survey of spiral galaxies – X. Surface photometry, decompositions and the Tully–Fisher relation in theR_cband

Adaptive optics for high resolution spectroscopy: a direct application with the future NIRPS spectrograph

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The effects of seeing on Sérsic profiles - II. The Moffat PSF

Cited by 191 publications

References 17 publications

A PHYSICAL APPROACH TO THE IDENTIFICATION OF HIGH-ZMERGERS: MORPHOLOGICAL CLASSIFICATION IN THE STELLAR MASS DOMAIN

A PHYSICAL APPROACH TO THE IDENTIFICATION OF HIGH-ZMERGERS: MORPHOLOGICAL CLASSIFICATION IN THE STELLAR MASS DOMAIN

GHASP: an Hα kinematic survey of spiral galaxies – X. Surface photometry, decompositions and the Tully–Fisher relation in theRcband

Adaptive optics for high resolution spectroscopy: a direct application with the future NIRPS spectrograph

Contact Info

Product

Resources

About

GHASP: an Hα kinematic survey of spiral galaxies – X. Surface photometry, decompositions and the Tully–Fisher relation in theR_cband