Removing static aberrations from the active optics system of a wide-field telescope

Schipani, P.; Noethe, L.; Arcidiacono, Carmelo; Argomedo, Javier; Dall’Ora, M.; D’Orsi, Sergio; Farinato, Jacopo; Magrin, Demetrio; Marty, Laurent; Ragazzoni, Roberto; Umbriaco, Gabriele

doi:10.1364/josaa.29.001359

Cited by 41 publications

(33 citation statements)

References 34 publications

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“…M. Capaccioli, Capaccioli et al 2015) being performed at the ESO VST. The VST is a 2.6 m wide-field optical survey telescope, located at Cerro Paranal in Chile (Schipani et al 2012). The VST is equipped with the wide-field camera OmegaCam, spanning a 1×1degree 2 field of view in the optical wavelength range from 0.3 to 1.0 μm (Kuijken 2011).…”

Section: Observations Data Reduction and Analysismentioning

confidence: 99%

THE FORNAX DEEP SURVEY WITH VST. I. THE EXTENDED AND DIFFUSE STELLAR HALO OF NGC 1399 OUT TO 192 kpc

Iodice

Capaccioli

Grado

et al. 2016

ApJ

169

342

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We have started a new, deep multi-imaging survey of the Fornax cluster, dubbed the Fornax Deep Survey (FDS), at the VLT Survey Telescope (VST). In this paper we present the deep photometry inside two square degrees around the bright galaxy NGC1399 in the core of the cluster. We found that the core of the Fornax cluster is characterized by a very extended and diffuse envelope surrounding the luminous galaxy NGC1399: we map the surface brightness out to 33 arcmin (∼192 kpc) from the galaxy center and down to μ g ∼31 mag arcsec −2 in the g band. The deep photometry allows us to detect a faint stellar bridge in the intracluster region on the west side of NGC1399 and toward NGC1387. By analyzing the integrated colors of this feature, we argue that it could be due to the ongoing interaction between the two galaxies, where the outer envelope of NGC1387 on its east side is stripped away. By fitting the light profile, we found that there exists a physical break radius in the total light distribution at R=10 arcmin (∼58 kpc) that sets the transition region between the bright central galaxy and the outer exponential halo, and that the stellar halo contributes 60% of the total light of the galaxy (Section 3.5). We discuss the main implications of this work on the build-up of the stellar halo at the center of the Fornax cluster. By comparing with the numerical simulations of the stellar halo formation for the most massive bright cluster galaxies (i.e., M M 13 log 14, we find that the observed stellar halo mass fraction is consistent with a halo formed through the multiple accretion of progenitors with stellar mass in the range 10 8 -10 11 M e . This might suggest that the halo of NGC1399 has also gone through a major merging event. The absence of a significant number of luminous stellar streams and tidal tails out to 192 kpc suggests that the epoch of this strong interaction goes back to an early formation epoch. Therefore, different from the Virgo cluster, the extended stellar halo around NGC1399 is characterized by a more diffuse and well-mixed component, including the intracluster light.

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Section: Observations Data Reduction and Analysismentioning

confidence: 99%

THE FORNAX DEEP SURVEY WITH VST. I. THE EXTENDED AND DIFFUSE STELLAR HALO OF NGC 1399 OUT TO 192 kpc

Iodice

Capaccioli

Grado

et al. 2016

ApJ

169

342

View full text Add to dashboard Cite

show abstract

“…VST is a 2.6-m wide field optical survey telescope, located at Cerro Paranal in Chile (Schipani et al 2012), equipped with the wide field camera (1 × 1 degree 2 ) OmegaCam, having a pixel scale of 0.21 arcsec/pixel. Data reduction was performed by using the VST-Tube pipeline (Grado et al 2012;Capaccioli et al 2015) and the analysis was described in detail by Iodice et al (2016).…”

Section: Data: the Fornax Deep Survey With Vstmentioning

confidence: 99%

Intracluster Patches of Baryons in the Core of the Fornax Cluster

Iodice

Spavone

Cantiello

et al. 2017

ApJ

116

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In the core of the Fornax cluster, on the West side of NGC 1399, we have detected a previously unknown region of intra-cluster light (ICL). It is made up by several faint (µ r 28 − 29 mag/arcsec 2 ) patches of diffuse light. The bulk of the ICL is located in between the three bright galaxies in the core, NGC 1387, NGC 1379 and NGC 1381, at 10 ≤ R ≤ 40 arcmin (∼ 58 − 230 kpc) from the central galaxy NGC 1399. We show that the ICL is the counterpart in the diffuse light of the known over-density in the population of blue globular clusters (GCs). The total g-band luminosity of the ICL is L g 8.3 × 10 9 L , which is ∼ 5% of the total luminosity of NGC 1399. This is consistent with the fraction of the blue GCs in the same region of the cluster. The ICL has g − r ∼ 0.7 mag, which is similar to the colors in the halo of the bright galaxies in the cluster core. The new findings were compared with theoretical predictions for the ICL formation and they support a scenario in which the intra-cluster population detected in the core of the Fornax cluster is build up by the tidal stripping of material (stars and GCs) from galaxy outskirts in a close passage with the cD. Moreover, the diffuse form of the ICL and its location close to the core of the cluster is expected in a dynamically evolved cluster as Fornax.

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“…Within each subfield the extreme data are eliminated by a median filter and the remaining data are averaged over the subfields. Figure 13 shows such a pattern of ellipticities e based on a 30-s exposure with the VST after an active optics correction under average seeing conditions [15]. Obviously, the pattern is different from the one of the perfect system shown in Figure 8.…”

Section: Elimination Of Outliers and Averaging Across Subfieldsmentioning

confidence: 91%

A method for the use of ellipticities and spot diameters for the measurement of aberrations in wide-field telescopes

Noethe¹,

Schipani

Holzlöhner

et al. 2014

Advanced Optical Technologies

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In wide-field survey telescopes, the patterns of spot sizes and ellipticities can be used to determine wavefront aberrations generated by the telescope. The calculation of spot sizes and ellipticities generated by telescope aberrations is most conveniently done if the aberrations are expressed in terms of Zernike-type polynomials whose derivatives are orthonormal. The field dependence of the spot sizes and ellipticities generated by the telescope can conveniently be expressed by low-order Zernike polynomials. Because the exposure times in astronomical survey work are typically rather short, this information may be used for a quasi-closed loop control of the telescope optics. The ability to accurately subtract ellipticities generated by telescope errors could also be useful for observations such as gravitational lensing surveys.

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Removing static aberrations from the active optics system of a wide-field telescope

Cited by 41 publications

References 34 publications

THE FORNAX DEEP SURVEY WITH VST. I. THE EXTENDED AND DIFFUSE STELLAR HALO OF NGC 1399 OUT TO 192 kpc

THE FORNAX DEEP SURVEY WITH VST. I. THE EXTENDED AND DIFFUSE STELLAR HALO OF NGC 1399 OUT TO 192 kpc

Intracluster Patches of Baryons in the Core of the Fornax Cluster

A method for the use of ellipticities and spot diameters for the measurement of aberrations in wide-field telescopes

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