Passively Evolving Early‐Type Galaxies at 1.4 ≲<i>z</i>≲ 2.5 in the Hubble Ultra Deep Field

Daddi, E.; Renzini, A.; Pirzkal, Norbert; Cimatti, A.; Malhotra, Sangeeta; Stiavelli, M.; Xu, Chun; Pasquali, A.; Rhoads, James E.; Brusa, M.; Alighieri, S. di Serego; Ferguson, Henry C.; Koekemoer, Anton M.; Moustakas, Leonidas A.; Panagia, N.; Windhorst, Rogier A.

doi:10.1086/430104

Cited by 881 publications

(1,107 citation statements)

References 89 publications

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“…Daddi et al 2005;Longhetti et al 2007;van Dokkum et al 2008;Trujillo et al 2006Trujillo et al , 2007. This itself is not a problem since an evolution in the M − Re relation is expected due to galaxies at later times being formed through less dissipative events (i.e.…”

Section: Comparison With High Redshift Datamentioning

confidence: 99%

Galaxy And Mass Assembly (GAMA): $\mathcal {M_\star }\text{--}R_{\rm e}$ relations ofz= 0 bulges, discs and spheroids

Lange

Moffett

Driver

et al. 2016

Mon. Not. R. Astron. Soc.

117

131

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Section: Comparison With High Redshift Datamentioning

confidence: 99%

Galaxy And Mass Assembly (GAMA): $\mathcal {M_\star }\text{--}R_{\rm e}$ relations ofz= 0 bulges, discs and spheroids

Lange

Moffett

Driver

et al. 2016

Mon. Not. R. Astron. Soc.

117

131

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“…Apart from the 4000 Å and 3600 Å Balmer break (which are at λ > 1 μm for z > 1.4 galaxies), another strong age-dependent feature in the UV is a break in the region 2640-2850 Å, which is produced by the combination of several strong absorption lines, including Mg iiλ2800. Daddi et al (2005) named this feature Mg UV and defined it to be the ratio of (two times) the flux at 2625 < λ < 2725 Å to the flux in two 100 Å broad regions above and below this range. Daddi et al show that only stellar populations older than 0.1 (0.4) Gyr have Mg UV significantly above 1.1 (1.4).…”

Section: Composite Spectramentioning

confidence: 99%

GMASS ultradeep spectroscopy of galaxies at z ~ 2

Kurk

Cimatti

Zamorani

et al. 2009

A&A

Self Cite

108

142

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Context. Clusters of galaxies represent important laboratories for studying galaxy evolution and formation. Well established and relaxed clusters are known below z < 1.4, as well as, clusters in formation found close to radio galaxies at z > 2, but the in-between redshift range, during which clusters are expected to undergo significant changes, is almost unexplored. Aims. By studying a galaxy overdensity in redshift and angular distribution at z = 1.6, uncovered in the Galaxy Mass Assembly ultra-deep Spectroscopic Survey (GMASS), we provide insight into the evolution of cluster galaxies at high redshift. Methods. We present a study of the significance of the galaxy overdensity at z = 1.6, Cl 0332-2742, its velocity dispersion, and X-ray emission. We identify the colour bimodality of the cluster members and compare the properties of members of Cl 0332-2742 with galaxies outside the overdensity. Results. From the redshifts of the 42 overdensity members, we measure a velocity dispersion of 500 km s −1 . We conservatively estimate the overdensity in redshift space for the spike at z = 1.6 in the GMASS field to be 8.3 ± 1.5. A map of the surface density of galaxies at z = 1.6 in the GMASS field shows that its structure is irregular with several filaments and local overdensities. The differences in the physical properties of Cl 0332-2742 member and field galaxies agree with the latest hierarchical galaxy formation models: for overdensity members, the star formation rate (SFR), and specific SFR, is approximately 50% lower than for the field galaxies; overdensity galaxies are twice the age, on average, of field galaxies; and there is a higher proportion of both massive (M > 10 10.7 M ), and early-type galaxies, inside Cl 0332-2742 than in the field. Among the 42 members, seven have spectra consistent with being passively evolving, massive galaxies. These are all located within an area where the surface density of z = 1.6 galaxies is highest. In a z − J colour-magnitude diagram, the photometric data of these early-type galaxies are in close agreement with a theoretical red sequence of a galaxy cluster at redshift z = 1.6, which formed most of its stars in a short burst of star formation at z ∼ 3. Conclusions. We conclude that the redshift spike at z = 1.6 in the GMASS field represents a sheet-like structure in the cosmic web, and that the area with the highest surface density within this structure, containing already seven passively evolving galaxies, will evolve into a cluster of galaxies at a later time.

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“…Massive early-type galaxies (ETGs) are found to be much more compact in the past than in the present Universe (Daddi et al 2005;Trujillo et al 2006;Trujillo et al 2007; van der Wel et al…”

Section: Introductionmentioning

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.

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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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Passively Evolving Early‐Type Galaxies at 1.4 ≲z≲ 2.5 in the Hubble Ultra Deep Field

Cited by 881 publications

References 89 publications

Galaxy And Mass Assembly (GAMA): $\mathcal {M_\star }\text{--}R_{\rm e}$ relations ofz= 0 bulges, discs and spheroids

Galaxy And Mass Assembly (GAMA): $\mathcal {M_\star }\text{--}R_{\rm e}$ relations ofz= 0 bulges, discs and spheroids

GMASS ultradeep spectroscopy of galaxies at z ~ 2

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

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