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

Iodice, E.; Capaccioli, M.; Grado, A.; Limatola, L.; Spavone, M.; Napolitano, N. R.; Paolillo, M.; Peletier, Reynier F.; Cantiello, M.; Lisker, Thorsten; Wittmann, Carolin; Venhola, Aku; Hilker, M.; D’Abrusco, R.; Pota, Vincenzo; Schipani, P.

doi:10.3847/0004-637x/820/1/42

Cited by 174 publications

(370 citation statements)

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“…The pixel size is 0.21 arcsec and the average FWHM of the observations is ≈ 1 arcsec, so that the PSF is well sampled. For further information about the data see Iodice et al (2016) and Peletier et al (in prep. ).…”

Section: Datamentioning

confidence: 99%

“…The red cross shows the cD galaxy NGC 1399 (see Iodice et al 2016) in the core of the Fornax cluster, and the blue cross shows the elliptical shell galaxy NGC 1316(see Iodice et al 2017) , which is the central galaxy of the Fornax-SW subcluster.…”

Section: Datamentioning

confidence: 99%

“…It covers a larger field-of-view than any of the previous Fornax surveys with deep multi-band observations, and has similar depth as the Next Generation Virgo Survey (Ferrarese et al 2012). The survey has already obtained several results, such as the discovery of an extended globular cluster population (D'Abrusco et al 2016), the characterization of the extended stellar halo of NGC 1399 (Iodice et al 2016), and the analysis of the merger system around NGC 1316 (Iodice et al 2017). Since we have deep data in g', r' and i'-bands, we can determine also the colors of the galaxies.…”

Section: Introductionmentioning

confidence: 98%

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The Fornax Deep Survey with VST

Venhola

Peletier

Laurikainen

et al. 2017

A&A

166

236

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Context. Studies of low surface brightness (LSB) galaxies in nearby clusters have revealed a sub-population of extremely diffuse galaxies with central surface brightness of µ 0,g > 24 mag arcsec −2 , total luminosity M g fainter than -16 mag and effective radius between 1.5 kpc < R e < 10 kpc. The origin of these Ultra Diffuse Galaxies (UDGs) is still unclear, although several theories have been suggested. As the UDGs overlap with the dwarf-sized galaxies in their luminosities, it is important to compare their properties in the same environment. If a continuum is found between the properties of UDGs and the rest of the LSB population, it would be consistent with the idea that they have a common origin. Aims. Our aim is to exploit the deep g', r' and i'-band images of the Fornax Deep Survey (FDS), in order to identify LSB galaxies in an area of 4 deg 2 in the center of the Fornax cluster. The identified galaxies are divided into UDGs and dwarf-sized LSB galaxies, and their properties are compared. Methods. We identify visually all extended structures having r'-band central surface brightness of µ 0,r > 23 mag arcsec −2 . We classify the objects based on their appearance into galaxies and tidal structures, and perform 2D Sérsic model fitting with GALFIT to measure the properties of those classified as galaxies. We analyze their radial distribution and orientations with respect of the cluster center, and with respect to the other galaxies in our sample. We also study their colors and compare the LSB galaxies in Fornax with those in other environments. Results. Our final sample complete in the parameter space of the previously known UDGs, consists of 205 galaxies of which 196 are LSB dwarfs (with R e < 1.5kpc) and 9 are UDGs (R e > 1.5 kpc). We show that the UDGs have (1) g'-r' colors similar to those of LSB dwarfs of the same luminosity. (2) The largest UDGs (R e >3kpc) in our sample appear different from the other LSB galaxies, in that they are significantly more elongated and extended, whereas (3) the smaller UDGs differ from the LSB dwarfs only by having slightly larger effective radii. (4) We do not find clear differences between the structural parameters of the UDGs in our sample and those of UDGs in other galaxy environments. (5) We find that the dwarf LSB galaxies in our sample are less concentrated in the cluster center than the galaxies with higher surface brightness, and that their number density drops within 180 kpc from the cluster center. We also compare the LSB dwarfs in Fornax with the LSB dwarfs in the Centaurus group, where data of similar quality to ours is available. (6) We find the smallest LSB dwarfs to have similar colors, sizes and Sérsic profiles regardless of their environment. However, in the Centaurus group the colors become bluer with increasing galaxy magnitudes, an effect which is probably due to smaller mass and hence weaker environmental influence of the Centaurus group. Conclusions. Our findings are consistent with the small UDGs forming the tail of a continuous distribution...

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Section: Datamentioning

confidence: 99%

Section: Datamentioning

confidence: 99%

Section: Introductionmentioning

confidence: 98%

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The Fornax Deep Survey with VST

Venhola

Peletier

Laurikainen

et al. 2017

A&A

166

236

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“…Gonzalez et al 2005; Da Rocha & Mendes de Oliveira 2005; Presotto et al 2014;Bender et al 2015;Iodice et al 2016, among many); see Peng et al (2011) for a more complete listing of earlier literature.…”

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confidence: 99%

Detection of the Stellar Intracluster Medium in Perseus (Abell 426)

Harris

Mulholland

2017

ApJ

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Hubble Space Telescope photometry from the ACS/WFC and WFPC2 cameras is used to detect and measure globular clusters (GCs) in the central region of the rich Perseus cluster of galaxies. A detectable population of Intragalactic GCs is found extending out to at least 500 kpc from the cluster center. These objects display luminosity and color (metallicity) distributions that are entirely normal for GC populations. Extrapolating from the limited spatial coverage of the HST fields, we estimate very roughly that the entire Perseus cluster should contain ∼ 50000 or more IGCs, but a targetted wide-field survey will be needed for a more definitive answer. Separate brief results are presented for the rich GC systems in NGC 1272 and NGC 1275, the two largest Perseus ellipticals. For NGC 1272 we find a specific frequency S N ≃ 8, while for the central giant NGC 1275, S N ≃ 12. In both these giant galaxies, the GC colors are well matched by bimodal distributions, with the majority in the blue (metal-poor) component. This preliminary study suggests that Perseus is a prime target for a more comprehensive deep imaging survey of Intragalactic GCs.

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“…The library of PSFs (FITS files) is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/601/A86 more distant ones (Mihos et al 2005;Martínez-Delgado et al 2010;Janowiecki et al 2010;Duc et al 2015;Iodice et al 2016). New imaging techniques have been developed (Mihos et al 2005;Ferrarese et al 2012;van Dokkum et al 2014), which enable us to reach the very low surface brightness levels needed to investigate the extended stellar structures of galaxies.…”

Section: Introductionmentioning

confidence: 99%

A deconvolution technique to correct deep images of galaxies from instrumental scattered light

Karabal

Duc

Küntschner

et al. 2017

A&A

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Deep imaging of the diffuse light that is emitted by stellar fine structures and outer halos around galaxies is often now used to probe their past mass assembly. Because the extended halos survive longer than the relatively fragile tidal features, they trace more ancient mergers. We use images that reach surface brightness limits as low as 28.5−29 mag arcsec −2 (g-band) to obtain light and color profiles up to 5-10 effective radii of a sample of nearby early-type galaxies. These were acquired with MegaCam as part of the CFHT MATLAS large programme. These profiles may be compared to those produced using simulations of galaxy formation and evolution, once corrected for instrumental effects. Indeed they can be heavily contaminated by the scattered light caused by internal reflections within the instrument. In particular, the nucleus of galaxies generates artificial flux in the outer halo, which has to be precisely subtracted. We present a deconvolution technique to remove the artificial halos that makes use of very large kernels. The technique, which is based on PyOperators, is more time efficient than the model-convolution methods that are also used for that purpose. This is especially the case for galaxies with complex structures that are hard to model. Having a good knowledge of the point spread function (PSF), including its outer wings, is critical for the method. A database of MegaCam PSF models corresponding to different seeing conditions and bands was generated directly from the deep images. We show that the difference in the PSFs in different bands causes artificial changes in the color profiles, in particular a reddening of the outskirts of galaxies having a bright nucleus. The method is validated with a set of simulated images and applied to three representative test cases: NGC 3599, NGC 3489, and NGC 4274, which exhibits a prominent ghost halo for two of them. This method successfully removes this.

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

Cited by 174 publications

References 74 publications

The Fornax Deep Survey with VST

The Fornax Deep Survey with VST

Detection of the Stellar Intracluster Medium in Perseus (Abell 426)

A deconvolution technique to correct deep images of galaxies from instrumental scattered light

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