Colour gradients in cluster ellipticals at z ∼ 1.4: the hidden content of the galaxy central regions

Ciocca, F.; Saracco, P.; Gargiulo, A.; Propris, Roberto De

doi:10.1093/mnras/stx003

Cited by 8 publications

(13 citation statements)

References 92 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The parameters of all the galaxies in these three clusters have been homogeneously derived using Galfit on ACS-F850LP images, sampling the rest-frame B-band at the redshift of the clusters. In particular, photometry and structural parameters of galaxies have been derived and studied by Saracco et al (2014) for cluster RXJ0848, by Ciocca et al (2017) for cluster XMMJ2235 and by Saracco et al (2017) for cluster XLSS0223. Jørgensen et al (2014) find a good agreement between their measurements for cluster RXJ0848 and those by Saracco et al (2014).…”

Section: High-redshift Samplementioning

confidence: 99%

See 1 more Smart Citation

The Fundamental Plane of cluster spheroidal galaxies at z ∼ 1.3: evidence for mass-dependent evolution

Saracco

Gargiulo

Barbera

et al. 2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We present spectroscopic observations obtained at the Large Binocular Telescope in the field of the cluster XLSSJ0223-0436 at z = 1.22. We confirm 12 spheroids cluster members and determine stellar velocity dispersion for 7 of them. We combine these data with those in the literature for clusters RXJ0848+4453 at z = 1.27 (8 galaxies) and XMMJ2235-2557 at z = 1.39 (7 galaxies) to determine the Fundamental Plane of cluster spheroids. We find that the FP at z ∼ 1.3 is offset and rotated (∼ 3σ) with respect to the local FP. The offset corresponds to a mean evolution ∆log(M dyn /L B )=(-0.5±0.1)z. High-redshift galaxies follow a steeper mass-dependenthigher-mass galaxies (log(M dyn /M ⊙ )≥11.5) have a higher-formation redshift (z f ≥6.5) than lower-mass ones (z f ≤2 for log(M dyn /M ⊙ ≤10)), with a median z f ≃ 2.5 for the whole sample. Also, galaxies with higher stellar mass density host stellar populations formed earlier than those in lower density galaxies. At fixed IMF, M dyn /M * varies systematically with mass and mass density. It follows that the evolution of the stellar populations (M * /L B ) accounts for the observed evolution of M dyn /L B for M dyn > 10 11 M ⊙ galaxies, while accounts for ∼85% of the evolution at M dyn < 10 11 M ⊙ . We find no evidence in favour of structural evolution of individual galaxies, while we find evidences that spheroids later added to the population may account for the observed discrepancy between ∆log(M dyn /L B ) and ∆ log(M * /L B ) at masses < 10 11 M ⊙ . Thus, the evolution of the FP of cluster spheroids is consistent with the mass-dependent and mass density-dependent evolution of their stellar populations superimposed to a minor contribution of spheroids joining the population at later times.

show abstract

Section: High-redshift Samplementioning

confidence: 99%

“…In the same Appendix, simulations dedicated to estimate the errors on the above parameters are also described, while Appendix C is dedicated to a comparison with Chan et al (2016) measurements showing a good agreement with their published measurements (see Fig. C2 of Ciocca et al 2017).…”

Section: Appendix A: High-redshift Cluster Samplementioning

confidence: 99%

The Fundamental Plane of cluster spheroidal galaxies at z ∼ 1.3: evidence for mass-dependent evolution

Saracco

Gargiulo

Barbera

et al. 2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…All massive galaxies out to r ∼ 1.5 Mpc have low SFRs, and those in the centre have lower specific SFRs than the rest of the population with the same mass (Grützbauch et al 2012). For the structural properties, this cluster has been investigated by Strazzullo et al (2010) and was also included in the cluster samples of Delaye et al (2014), De Propris et al (2015) and Ciocca et al (2017).…”

Section: The Kcs Samplementioning

confidence: 99%

“…Tamura & Ohta 2003) also showed that color gradients may be preferentially produced by radial variation in metallicity rather than age. At z > 1, studies of color gradients are limited (see, for example Gargiulo et al 2012;De Propris et al 2015Ciocca et al 2017). In Chan et al (2016) we quantitatively investigated the evolution of color gradients in XMMU J2235-2557 by modeling the inner (defined to be the color at 0.5a e ) and outer (2.0a e ) regions of the galaxies under different assumptions of the radial variation of stellar population properties, using stellar population models of Bruzual & Charlot (2003).…”

Section: The Evolution Of Ratio Of Mass-weighted To Light-weighted Sizesmentioning

confidence: 99%

“…Another caveat is that our analysis is based on a single color gradient. Recent work by Ciocca et al (2017) measured the rest-frame UV −U gradients (via ∇ i 775 −z 850 ) as well as ∇ z 850 −H 160 in XMMU J2235-2557. While their ∇ z 850 −H 160 gradients are negative and roughly consistent with our work (the discrepancies may result from the depth of data they used and the methodology), they also found positive rest-frame UV −U gradients, which cannot be simultaneously explained by an age, metallicity or dust gradient.…”

Section: The Evolution Of Ratio Of Mass-weighted To Light-weighted Sizesmentioning

confidence: 99%

See 1 more Smart Citation

The KMOS Cluster Survey (KCS). II. The Effect of Environment on the Structural Properties of Massive Cluster Galaxies at Redshift 1.39 < z < 1.61*

Chan

Beifiori

Saglia

et al. 2018

ApJ

View full text Add to dashboard Cite

We present results on the structural properties of massive passive galaxies in three clusters at 1.39 < z < 1.61 from the KMOS Cluster Survey. We measure light-weighted and mass-weighted sizes from optical and nearinfrared Hubble Space Telescope imaging and spatially resolved stellar mass maps. The rest-frame R-band sizes of these galaxies are a factor of ∼ 2 − 3 smaller than their local counterparts. The slopes of the relation between the stellar mass and the light-weighted size are consistent with recent studies in clusters and the field. Their mass-weighted sizes are smaller than the rest frame R-band sizes, with an average mass-weighted to light-weighted size ratio that varies between ∼ 0.45 and 0.8 among the clusters. We find that the median light-weighted size of the passive galaxies in the two more evolved clusters is ∼ 24% larger than for field galaxies, independent of the use of circularized effective radii or semi-major axes. These two clusters also show a smaller size ratio than the less evolved cluster, which we investigate using color gradients to probe the underlying M * /L H 160 gradients. The median color gradients are ∇z − H ∼ −0.4 mag dex −1 , twice the local value. Using stellar populations models, these gradients are best reproduced by a combination of age and metallicity gradients. Our results favor the minor merger scenario as the dominant process responsible for the observed galaxy properties and the environmental differences at this redshift. The environmental differences support that clusters experience accelerated structural evolution compared to the field, likely via an epoch of enhanced minor merger activity during cluster assembly.

show abstract

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Boissier

Cucciati

Boselli

et al. 2018

A&A

View full text Add to dashboard Cite

Context. At low redshift, early-type galaxies often exhibit a rising flux with decreasing wavelength in the 1000–2500 Å range, called “UV upturn”. The origin of this phenomenon is debated, and its evolution with redshift is poorly constrained. The observed GALEX FUV-NUV color can be used to probe the UV upturn approximately to redshift 0.5.Aim. We provide constraints on the existence of the UV upturn up to redshift ~0.4 in the brightest cluster galaxies (BCG) located behind the Virgo cluster, using data from the GUViCS survey.Methods. We estimate the GALEX far-UV (FUV) and near-UV (NUV) observed magnitudes for BCGs from the maxBCG catalog in the GUViCS fields. We increase the number of nonlocal galaxies identified as BCGs with GALEX photometry from a few tens of galaxies to 166 (64 when restricting this sample to relatively small error bars). We also estimate a central color within a 20 arcsec aperture. By using the r-band luminosity from the maxBCG catalog, we can separate blue FUV-NUV due to recent star formation and candidate upturn cases. We use Lick indices to verify their similarity to redshift 0 upturn cases.Results. We clearly detect a population of blue FUV-NUV BCGs in the redshift range 0.10–0.35, vastly improving the existing constraints at these epochs by increasing the number of galaxies studied, and by exploring a redshift range with no previous data (beyond 0.2), spanning one more Gyr in the past. These galaxies bring new constraints that can help distinguish between assumptions concerning the stellar populations causing the UV upturn phenomenon. The existence of a large number of UV upturns around redshift 0.25 favors the existence of a binary channel among the sources proposed in the literature.

show abstract

Colour gradients in cluster ellipticals at z ∼ 1.4: the hidden content of the galaxy central regions

Cited by 8 publications

References 92 publications

The Fundamental Plane of cluster spheroidal galaxies at z ∼ 1.3: evidence for mass-dependent evolution

The Fundamental Plane of cluster spheroidal galaxies at z ∼ 1.3: evidence for mass-dependent evolution

The KMOS Cluster Survey (KCS). II. The Effect of Environment on the Structural Properties of Massive Cluster Galaxies at Redshift 1.39 < z < 1.61*

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Contact Info

Product

Resources

About