SPIDER - I. Sample and galaxy parameters in the grizYJHK wavebands

Barbera, F. La; Carvalho, R. R. de; Rosa, I. G. de la; Lopes, P. A. A.; Kohl-Moreira, J. L.; Capelato, H. V.

doi:10.1111/j.1365-2966.2010.16850.x

Cited by 132 publications

(200 citation statements)

References 62 publications

(69 reference statements)

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“…In order to study the evolution of mass-weighted sizes over redshift, we compare our cluster sample at z ∼ 1.39 to a local sample of passive galaxies from the Spheroids Panchromatic Investigation in Different Environmental Regions (SPIDER) survey (La Barbera et al 2010b). The publicly available SPIDER sample includes 39993 passive galaxies selected from SDSS Data Release 6 (DR6), among them 5080 are in the near-infrared UKIRT Infrared Deep Sky Survey-Large Area Survey Data release (UKIDSS-LAS DR4) in the redshift range of 0.05 to 0.095.…”

Section: Local Comparison Samplementioning

confidence: 99%

“…The publicly available SPIDER sample includes 39993 passive galaxies selected from SDSS Data Release 6 (DR6), among them 5080 are in the near-infrared UKIRT Infrared Deep Sky Survey-Large Area Survey Data release (UKIDSS-LAS DR4) in the redshift range of 0.05 to 0.095. La Barbera et al (2010b) derived structural parameters in all available bands (grizY JHK) with single Sérsic fitting with 2DPhot (La Barbera et al 2008).…”

Section: Local Comparison Samplementioning

confidence: 99%

“…For the galaxy selection, we follow similar criteria as La Barbera et al (2010b): we apply a magnitude cut at the 95% completeness magnitude (M r −20.55), a χ 2 cut from the Sérsic fit for both gband and r-band (χ 2 < 2.0), and a seeing cut at 1.5". This results in a sample of 4050 objects.…”

Section: Local Comparison Samplementioning

confidence: 99%

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Sizes, colour gradients and resolved stellar mass distributions for the massive cluster galaxies in XMMUJ2235-2557 atz= 1.39

Chan

Beifiori

Mendel

et al. 2016

Mon. Not. R. Astron. Soc.

137

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(2016) 'Sizes, colour gradients and resolved stellar mass distributions for the massive cluster galaxies in XMMUJ2235-2557 at z = 1.39.', Monthly notices of the Royal Astronomical Society., 458 (3). pp. 3181-3209. Further information on publisher's website: Additional information: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-pro t purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. ABSTRACTWe analyse the sizes, colour gradients, and resolved stellar mass distributions for 36 massive and passive galaxies in the cluster XMMUJ2235-2557 at z = 1.39 using optical and nearinfrared Hubble Space Telescope imaging. We derive light-weighted Sérsic fits in five HST bands (i 775 , z 850 ,Y 105 , J 125 , H 160 ), and find that the size decreases by ∼ 20% going from i 775 to H 160 band, consistent with recent studies. We then generate spatially resolved stellar mass maps using an empirical relationship between M * /L H 160 and (z 850 − H 160 ) and use these to derive mass-weighted Sérsic fits: the mass-weighted sizes are ∼ 41% smaller than their restframe r-band counterparts compared with an average of ∼ 12% at z ∼ 0. We attribute this evolution to the evolution in the M * /L H 160 and colour gradient. Indeed, as expected, the ratio of mass-weighted to light-weighted size is correlated with the M * /L gradient, but is also mildly correlated with the mass surface density and mass-weighted size. The colour gradients (∇ z−H ) are mostly negative, with a median value of ∼ 0.45 mag dex −1 , twice the local value. The evolution is caused by an evolution in age gradients along the semi-major axis (a), with ∇ age = d log(age)/d log(a) ∼ −0.33, while the survival of weaker colour gradients in old, local galaxies implies that metallicity gradients are also required, with ∇ Z = d log(Z)/d log(a) ∼ −0.2. This is consistent with recent observational evidence for the inside-out growth of passive galaxies at high redshift, and favours a gradual mass growth mechanism, such as minor mergers.

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Section: Local Comparison Samplementioning

confidence: 99%

Section: Local Comparison Samplementioning

confidence: 99%

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Sizes, colour gradients and resolved stellar mass distributions for the massive cluster galaxies in XMMUJ2235-2557 atz= 1.39

Chan

Beifiori

Mendel

et al. 2016

Mon. Not. R. Astron. Soc.

137

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“…Thus, we have finally gathered those systems with the highest S/N in the r-band images, S/N r ≡ 1/MAGERR_AUTO_r> 50 (La Barbera et al 2008Barbera et al , 2010Roy et al 2016, in preparation). This sample consists of ∼ 380 000 galaxies.…”

Section: Kids High Signal-to-noise Galaxy Samplementioning

confidence: 99%

Towards a census of supercompact massive galaxies in the Kilo Degree Survey

Tortora¹,

Barbera²,

Napolitano³

et al. 2016

Mon. Not. R. Astron. Soc.

Self Cite

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The abundance of compact, massive, early-type galaxies (ETGs) provides important constraints to galaxy formation scenarios. Thanks to the area covered, depth, excellent spatial resolution and seeing, the ESO Public optical Kilo Degree Survey (KiDS), carried out with the VLT Survey Telescope (VST), offers a unique opportunity to conduct a complete census of the most compact galaxies in the Universe. This paper presents a first census of such systems from the first 156 square degrees of KiDS. Our analysis relies on g-, r-, and i-band effective radii (R e ), derived by fitting galaxy images with PSF-convolved Sérsic models, high-quality photometric redshifts, z phot , estimated from machine learning techniques, and stellar masses, M ⋆ , calculated from KiDS aperture photometry. After massiveness (M ⋆ > ∼ 8 × 10 10 M ⊙ ) and compactness (R e ∼ < 1.5 kpc in g-, r-and ı-bands) criteria are applied, a visual inspection of the candidates plus near-infrared photometry from VIKING-DR1 are used to refine our sample. The final catalog, to be spectroscopically confirmed, consists of 92 systems in the redshift range z ∼ 0.2 − 0.7. This sample, which we expect to increase by a factor of ten over the total survey area, represents the first attempt to select massive super-compact ETGs (MSCGs) in KiDS. We investigate the impact of redshift systematics in the selection, finding that this seems to be a major source of contamination in our sample. A preliminary analysis shows that MSCGs exhibit negative internal colour gradients, consistent with a passive evolution of these systems. We find that the number density of MSCGs is only mildly consistent with predictions from simulations at z > 0.2, while no such system is found at z < 0.2.

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“…LogM > 10.64 and σ e > ∼ 110 km s −1 ; we have already stated in the Introduction that all the trends found in local Universe are similar). Specifically, Tortora et al (2013) derived, assuming different dark matter (DM) profiles, the Γ values for ∼4500 giant ETGs drawn from the SPIDER project (La Barbera et al 2010) in the redshift range of z = 0.05−0.1. The SPIDER sample is 95% complete at a stellar mass M = 3 × 10 10 M , which corresponds to σ ∼ 160 km s −1 .…”

Section: Imf-σ Trend In Local Universementioning

confidence: 99%

Lower mass normalization of the stellar initial mass function for dense massive early-type galaxies atz~ 1.4

Gargiulo

Saracco

Longhetti

et al. 2015

A&A

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Aims. This paper aims at understanding whether the normalization of the stellar initial mass function (IMF) of massive galaxies varies with cosmic time and/or with mean stellar mass density Σ = M /(2πR 2 e ). Methods. We have tackled this question by taking advantage of a spectroscopic sample of 18 dense (Σ > 2500 M pc −2 ) massive early-type galaxies (ETGs) that we collected at 1.2 < ∼ z < ∼ 1.6. Each galaxy in the sample was selected in order to have available: i) a high-resolution deep HST-F160W image to visually classify it as an ETG; ii) an accurate velocity dispersion estimate; iii) stellar mass derived through the fit of multiband photometry; and iv) structural parameters (i.e. effective radius R e and Sersic index n) derived in the F160W-band. We have constrained the mass-normalization of the IMF of dense high-z ETGs by comparing the true stellar masses of the ETGs in the sample (M true ) derived through virial theorem, hence IMF independent, with those inferred through the fit of the photometry which assume a reference IMF (M ref ). Adopting the virial estimator as proxy of the true stellar mass, we have implicitly assumed that these systems have zero dark matter. However, recent dynamical analysis of massive local ETGs have shown that the dark matter fraction within R e in dense ETGs is negligible (<5−10%) and simulations of dissipationless mergers of spheroidal galaxies have shown that this fraction decreases going back with time. Accurate dynamical models of local ETGs performed by the ATLAS 3D team have shown that the virial estimator is prone to underestimating or overestimating the total masses. We have considered this, and based on the results of ATLAS 3D we have shown that for dense ETGs the mean value of total masses derived through the virial estimator with a non-homologous virial coefficient and Sersic-R e are perfectly in agreement with the mean value of those derived through more sophisticated dynamical models, although, of course, the estimates show higher uncertainties. Results. Tracing the variation of the parameter Γ = M true /M ref with velocity dispersion σ e , we have found that, on average, dense ETGs at z = 1.4 follow the same IMF-σ e trend of typical local ETGs, but with a lower mass-normalization. The observed lower normalization could be evidence of i) an evolution of the IMF with time or ii) a correlation with Σ. To discriminate between the two possibilities, we have compared the IMF-σ e trend that we have found for high-z dense ETGs with that of local ETGs with similar mean stellar mass density and velocity dispersion and we have found that the IMF of massive dense ETGs does not depend on redshift. The similarity between the IMF-σ e trends observed both in dense high-z and low-z ETGs over 9 Gyr of evolution and their lower massnormalization with respect to the mean value of local ETGs suggests that, independently of formation redshift, the physical conditions which characterized the formation of a dense spheroid on average lead to a mass spectrum of newly formed stars ...

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SPIDER - I. Sample and galaxy parameters in the grizYJHK wavebands

Cited by 132 publications

References 62 publications

Sizes, colour gradients and resolved stellar mass distributions for the massive cluster galaxies in XMMUJ2235-2557 atz= 1.39

Sizes, colour gradients and resolved stellar mass distributions for the massive cluster galaxies in XMMUJ2235-2557 atz= 1.39

Towards a census of supercompact massive galaxies in the Kilo Degree Survey

Lower mass normalization of the stellar initial mass function for dense massive early-type galaxies atz~ 1.4

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