J-PLUS: Analysis of the intracluster light in the Coma cluster

Jiménez-Teja, Y.; Dupke, Renato A.; Oliveira, R. Lopes de; Xavier, H. S.; Coelho, P.; Chies-Santos, Ana L.; López-Sanjuan, C.; Álvarez-Candal, A.; Costa-Duarte, M. V.; Telles, E.; Hernández-Jiménez, J. A.; Benı́tez, N.; Alcaniz, J. S.; Cenarro, J.; Cristóbal-Hornillos, D.; Ederoclite, A.; Marín-Franch, A.; Oliveira, C. Mendes de; Moles, M.; Sodré, L.; Varela, J.; Ramió, H. Vázquez

doi:10.1051/0004-6361/201833547

Cited by 45 publications

(39 citation statements)

References 77 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…We find ICL fractions in good agreement with the ones in Jiménez- Teja et al (2019) in the F606W and F814W filters. Our fraction in the F435W filter differs significantly (we find a value of 2.5% compared to their value of 7.22%), which can be due to a number of differences in the data processing, since the sky level is computed differently in both studies, and to the fact that these authors used a different analysis package CICLE (CHEFs Intracluster Light Estimator; Jiménez-Teja & Dupke 2016) to extract and remove galaxy light profiles.…”

Section: Resultssupporting

confidence: 83%

“…ICL has been found in nearby galaxy clusters such as the Virgo cluster (Mihos et al 2017) or the Coma cluster (Gu et al 2018;Jiménez-Teja et al 2019), in the form of an extended lumi-nous halo centered on the BCG, superposed on a variety of substructures such as straight streams (Mihos et al 2005), curved arcs (Trentham & Mobasher 1998), large plumes (Gregg & West 1998) or tidal tails (Krick et al 2006;Janowiecki et al 2010). However, due to the difficulty to quantify their morphological properties, the studies of such features remain mainly qualitative, as a disclosure of the numerous mechanisms occurring in the ICL.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

The complex case of MACS J0717.5+3745 and its extended filament: intra-cluster light, galaxy luminosity function, and galaxy orientations

Ellien

Durret

Adami

et al. 2019

A&A

View full text Add to dashboard Cite

Context. The properties of galaxies are known to be affected by their environment, but although galaxies in clusters and groups have been quite thoroughly investigated, little is known presently on galaxies belonging to filaments of the cosmic web, and on the properties of the filaments themselves. Aims. We investigate here the properties of the rich cluster MACS J0717.5+3745 and its extended filament, by analyzing the distribution and fractions of intra-cluster light (ICL) in the core of this cluster and by trying to detect intra-filament light (IFL) in the filament. We analyze the galaxy luminosity function (GLF) of the cluster core and of the filament. We also study the orientations of galaxies in the filament to better constrain the filament properties. Methods. This work is based on Hubble Space Telescope archive data, both from the Hubble Frontier Fields in the F435W, F606W, F814W, and F105W bands, and from a mosaic of images in the F606W and F814W bands. The spatial distribution of the ICL is determined with our new wavelet-based software, DAWIS. The GLFs are extracted in the F606W and F814W bands, with a statistical subtraction of the background, and fit with Schechter functions. The galaxy orientations in the filaments are estimated with SExtractor after correction for the Point Spread Function. Results. We detect a large amount of ICL in the cluster core, but no IFL in the cosmic filament. The fraction of ICL in the core peaks in the F606W filter before decreasing with wavelength. Though quite noisy, the GLFs in the filament are notably different from those of field galaxies, with a flatter faint end slope and an excess of bright galaxies. We do not detect a significant alignment of the galaxies in the filament region that was analyzed.

show abstract

Section: Resultssupporting

confidence: 83%

Section: Introductionmentioning

confidence: 99%

The complex case of MACS J0717.5+3745 and its extended filament: intra-cluster light, galaxy luminosity function, and galaxy orientations

Ellien

Durret

Adami

et al. 2019

A&A

View full text Add to dashboard Cite

show abstract

“…To date, Coma also appears in a more dynamical active phase. As observed in Fornax, the ICL distribution is more elongated in one direction (toward the east) and over a common envelope between the two giant galaxies in the core (Jiménez-Teja et al 2019). It is dominated by younger and low-metallicity stars, suggesting that this component could be formed by the stripping of stars from the galaxy outskirts and/or the disruption of dwarf galaxies during merging (see Jiménez-Teja et al 2019, and references therein).…”

Section: How Does Fornax Compare With Nearby Clusters?mentioning

confidence: 70%

The Fornax Deep Survey with the VST

Iodice

Spavone

Capaccioli

et al. 2019

A&A

192

View full text Add to dashboard Cite

Context. This paper is based on the multi-band (ugri) Fornax Deep Survey (FDS) with the VLT Survey Telescope (VST). We study bright early-type galaxies (mB ≤ 15 mag) in the 9 square degrees around the core of the Fornax cluster, which covers the virial radius (Rvir ∼ 0.7 Mpc). Aims. The main goal of the present work is to provide an analysis of the light distribution for all galaxies out to unprecedented limits (in radius and surface brightness) and to release the main products resulting from this analysis in all FDS bands. We give an initial comprehensive view of the galaxy structure and evolution as a function of the cluster environment. Methods. From the isophote fit, we derived the azimuthally averaged surface brightness profiles, the position angle, and ellipticity profiles as a function of the semi-major axis. In each band, we derived the total magnitudes, effective radii, integrated colours, and stellar mass-to-light ratios. Results. The long integration times, the arcsec-level angular resolution of OmegaCam at VST, and the large covered area of FDS allow us to map the light and colour distributions out to large galactocentric distances (up to about 10−15 Re) and surface brightness levels beyond μr = 27 mag arcsec−2 (μB ≥ 28 mag arcsec−2). Therefore, the new FDS data allow us to explore in great detail the morphology and structure of cluster galaxies out to the region of the stellar halo. The analysis presented in this paper allows us to study how the structure of galaxies and the stellar population content vary with the distance from the cluster centre. In addition to the intra-cluster features detected in previous FDS works, we found a new faint filament between FCC 143 and FCC 147, suggesting an ongoing interaction. Conclusions. The observations suggest that the Fornax cluster is not completely relaxed inside the virial radius. The bulk of the gravitational interactions between galaxies happens in the W-NW core region of the cluster, where most of the bright early-type galaxies are located and where the intra-cluster baryons (diffuse light and globular clusters) are found. We suggest that the W-NW sub-clump of galaxies results from an infalling group onto the cluster, which has modified the structure of the galaxy outskirts (making asymmetric stellar halos) and has produced the intra-cluster baryons (ICL and GCs), concentrated in this region of the cluster.

show abstract

“…(J0861), plus the filter on the Hα line (J0660). Thus, J-PLUS covers the whole optical wavelength range, enabling different kind of studies in stellar astrophysics (Bonatto et al 2019;Whitten et al 2019;Solano et al 2019), galaxies at several redshift ranges (Logroño-García et al 2019;San Roman et al 2019;Nogueira-Cavalcante et al 2019) or in clusters (Molino et al 2019;Jiménez-Teja et al 2019), and extreme Lyman-α emitters at z > 2 (Spinoso et al 2020).…”

Section: J-plus Photometric Datamentioning

confidence: 99%

J-PLUS: The star formation main sequence and rate density at d ≲ 75 Mpc

Vilella-Rojo

Logroño-García

López-Sanjuán

et al. 2021

A&A

Self Cite

View full text Add to dashboard Cite

Aims. Our goal is to estimate the star formation main sequence (SFMS) and the star formation rate density (SFRD) at z ≤ 0.017 (d 75 Mpc) using the Javalambre Photometric Local Universe Survey (J-PLUS) first data release, that probes 897.4 deg 2 with twelve optical bands. Methods. We extract the Hα emission flux of 805 local galaxies from the J-PLUS filter J0660, being the continuum level estimated with the other eleven J-PLUS bands, and the dust attenuation and nitrogen contamination corrected with empirical relations. Stellar masses (M), Hα luminosities (L Hα), and star formation rates (SFRs) were estimated by accounting for parameters covariances. Our sample comprises 689 blue galaxies and 67 red galaxies, classified in the (u − g) vs (g − z) color-color diagram, plus 49 AGN. Results. The SFMS is explored at log M 8 and it is clearly defined by the blue galaxies, with the red galaxies located below them. The SFMS is described as log SFR = 0.83 log M −8.44. We find a good agreement with previous estimations of the SFMS, especially those based on integral field spectroscopy. The Hα luminosity function of the AGN-free sample is well described by a Schechter function with log L * Hα = 41.34, log φ * = −2.43, and α = −1.25. Our measurements provide a lower characteristic luminosity than several previous studies in the literature. Conclusions. The derived star formation rate density at d 75 Mpc is log ρ SFR = −2.10 ± 0.11, with red galaxies accounting for 15% of the SFRD. Our value is lower than previous estimations at similar redshift, and provides a local reference for evolutionary studies regarding the star formation history of the Universe.

show abstract

J-PLUS: Analysis of the intracluster light in the Coma cluster

Cited by 45 publications

References 77 publications

The complex case of MACS J0717.5+3745 and its extended filament: intra-cluster light, galaxy luminosity function, and galaxy orientations

The complex case of MACS J0717.5+3745 and its extended filament: intra-cluster light, galaxy luminosity function, and galaxy orientations

The Fornax Deep Survey with the VST

J-PLUS: The star formation main sequence and rate density at d ≲ 75 Mpc

Contact Info

Product

Resources

About