A comprehensive study of large-scale structures in the GOODS-SOUTH field up to ${\mathsf z} \sim $ 2.5

Salimbeni, S.; Castellano, M.; Pentericci, L.; Trèvese, D.; Fiore, F.; Grazian, A.; Fontana, A.; Giallongo, E.; Boutsia, K.; Cristiani, S.; Santis, C. De; Gallozzi, S.; Menci, Nicola; Nonino, M.; Paris, D.; Santini, P.; Vanzella, E.

doi:10.1051/0004-6361/200811570

Cited by 47 publications

(74 citation statements)

References 72 publications

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“…Marchesini et al 2009;Eminian et al 2008;Lamareille et al 2008), the CB09 models give masses that are on average lower than the BC03 ones. In particular, the recent study by Salimbeni et al (2009) on a sample that partially overlaps with the present one showed that the average mass difference in their highest redshift bin (which includes the range z ∼ 2.5−3.5, see their Fig. 4) is around ∼30%, with a slight dependence on mass.…”

Section: Spectral Energy Distribution Fittingsupporting

confidence: 52%

Physical and morphological properties ofz~ 3 Lyman break galaxies: dependence on Lyαline emission

Pentericci¹,

Grazian²,

Scarlata

et al. 2010

A&A

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Aims. We investigate the physical and morphological properties of Lyman break galaxies (LBGs) at redshift ∼2.5 to ∼3.5, to determine if and how they depend on the nature and strength of the Lyα emission. Methods. We selected U-dropout galaxies from the z-detected GOODS-MUSIC catalog by adapting the classical Lyman break criteria on the GOODS filter set. We kept only those galaxies with spectroscopic confirmation, mainly from VIMOS and FORS public observations. Using the full multi-wavelength 14-bands information (U to IRAC), we determined the physical properties of the galaxies through a standard spectral energy distribution fitting procedure with the updated Charlot & Bruzual (2009) templates. We also added other relevant observations of the GOODS field, i.e. the 24 μm observations from Spitzer/MIPS and the 2 MSec Chandra X-ray observations. Finally, using non parametric diagnostics (Gini, Concentration, Asymmetry, M 20 and ellipticity), we characterized the rest-frame UV morphologies of the galaxies. We then analyzed how these physical and morphological properties correlate with the presence of the Lyα emission line in the optical spectra. Results. We find that unlike at higher redshift, the dependence of physical properties on the Lyα line is milder: galaxies without Lyα in emission tend to be more massive and dustier than the rest of the sample, but all other parameters, ages, star formation rates (SFR), X-ray emission and UV morphology do not depend strongly on the presence of the Lyα emission. A simple scenario where all LBGs have intrinsically high Lyα emission, but where the dust and neutral hydrogen content (which shapes the final appearance of the Lyα) depend on the mass of the galaxies, is able to reproduce the majority of the observed properties at z ∼ 3. Some modification might be needed to account for the observed evolution of these properties with cosmic epoch, which is also discussed.

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Section: Spectral Energy Distribution Fittingsupporting

confidence: 52%

Physical and morphological properties ofz~ 3 Lyman break galaxies: dependence on Lyαline emission

Pentericci¹,

Grazian²,

Scarlata

et al. 2010

A&A

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“…We overplot on Figure 5 the position of overdensities found in the GOODS-S field by Salimbeni et al (2009). These have been derived from the GOODS-MUSIC catalogue using a smoothed 3D density searching algorithm.…”

Section: Overdensities In the 3d-hst Deep Fieldsmentioning

confidence: 99%

“…In the COSMOS field (see Figure 6), Scoville et al (2007) applied an adaptive smoothing technique (similar to Salimbeni et al 2009) to find large scale structures at z < 1. While their results do not constrain the size of the structure and are less sensitive to very compact overdensities, we do find that their detections in the 3D-HST footprint correspond to high overdensities in our work.…”

Section: Overdensities In the 3d-hst Deep Fieldsmentioning

confidence: 99%

“…Black circles mark the position of X-Ray extended emission from Finoguenov et al (2015), the size of the circle representing the extension of the emission (R 200 ). Red circles mark the position of galaxy overdensities from Salimbeni et al (2009) who used a smoothed 3D density technique from the GOODS-MUSIC catalogue to search for overdensities (the size of the circle is arbitrary and fixed). Fontanot et al 2012;Guo et al 2013a).…”

Section: The Model Galaxy Samplementioning

confidence: 99%

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Galaxy Environment in the 3D-HST Fields: Witnessing the Onset of Satellite Quenching at z ∼ 1–2

Fossati

Wilman

Mendel

et al. 2017

ApJ

119

131

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We make publicly available a catalog of calibrated environmental measures for galaxies in the five 3D-HST/CANDELS deep fields. Leveraging the spectroscopic and grism redshifts from the 3D-HST survey, multi wavelength photometry from CANDELS, and wider field public data for edge corrections, we derive densities in fixed apertures to characterize the environment of galaxies brighter than JH 140 < 24 mag in the redshift range 0.5 < z < 3.0. By linking observed galaxies to a mock sample, selected to reproduce the 3D-HST sample selection and redshift accuracy, each 3D-HST galaxy is assigned a probability density function of the host halo mass, and a probability that is a central or a satellite galaxy. The same procedure is applied to a z = 0 sample selected from SDSS. We compute the fraction of passive central and satellite galaxies as a function of stellar and halo mass, and redshift, and then derive the fraction of galaxies that were quenched by environment specific processes. Using the mock sample, we estimate that the timescale for satellite quenching is t quench ∼ 2 − 5 Gyr; longer at lower stellar mass or lower redshift, but remarkably independent of halo mass. This indicates that, in the range of environments commonly found within the 3D-HST sample (M h 10 14 M ⊙ ), satellites are quenched by exhaustion of their gas reservoir in absence of cosmological accretion. We find that the quenching times can be separated into a delay phase during which satellite galaxies behave similarly to centrals at fixed stellar mass, and a phase where the star formation rate drops rapidly (τ f ∼ 0.4 − 0.6 Gyr), as shown previously at z = 0. We conclude that this scenario requires satellite galaxies to retain a large reservoir of multi-phase gas upon accretion, even at high redshift, and that this gas sustains star formation for the long quenching times observed.

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“…However, in our SAM we considered as groups structures with masses in the range 10 13.5 < M < 10 14.3 M and as clusters structures with mass M > 10 14.3 M . We note that selecting structures according to their mass makes little difference with data: in fact, the masses of groups or small clusters with σ < 700 km s −1 selected by Pentericci et al are of the order of 0.5 to few times 10 14 M (see also Salimbeni et al 2009). The predictions for the two modes are shown as shaded regions (see the figure caption for more details), up to redshift z ∼ 1 for groups and z ∼ 0.7 for clusters.…”

Section: Environmental Dependence: Agn In Groups and Clustersmentioning

confidence: 83%

Physical properties of AGN host galaxies as a probe of supermassive black hole feeding mechanisms

Gatti¹,

Lamastra²,

Menci³

et al. 2015

A&A

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Using an advanced semi-analytical model (SAM) for galaxy formation, we investigated the statistical effects of assuming two different mechanisms for triggering AGN activity on the properties of AGN host galaxies. We considered a first accretion mode where AGN activity is triggered by disk instabilities (DI) in isolated galaxies, and a second feeding mode where galaxy mergers and fly-by events (interactions, IT) are responsible for producing a sudden destabilization of large quantities of gas, causing the mass inflow onto the central supermassive black hole. The effects of including IT and DI modes in our SAM were studied and compared with observations separately to single out the regimes in which they might be responsible for triggering AGN activity. We obtained the following results: i) the predictions of our model concerning the stellar mass functions of AGN hosts point out that both DI and IT modes are able to account for the observed abundance of AGN host galaxies with M * < ∼ 10 11 M ; for more massive hosts, the DI scenario predicts a much lower space density than the IT model in every redshift bin, lying below the observational estimates for redshift z > 0.8. ii) The analysis of the colour−magnitude diagram of AGN hosts for redshift z < 1.5 can provide a good observational test to effectively distinguish between DI and IT mode, since DIs are expected to yield AGN host galaxy colours skewed towards bluer colours, while in the IT scenario the majority of hosts are expected to reside in the red sequence. iii) While both IT and DI scenarios can account for AGN triggered in main sequence or starburst galaxies, DIs fail in triggering AGN activity in passive galaxies. The lack of DI AGN in passive hosts is rather insensitive to changes in the model describing the DI mass inflow, and it is mainly caused by the criterion for the onset of disk instabilities included in our SAM. iv) The two modes are characterized by a different duration of the AGN phase, with DIs lasting even on time scales of ∼Gyr, much longer than in the IT scenario, where the galaxy interaction sets the duration of the burst phase around ∼10 7 −10 8 yr. v) The scatter of the star formation rate SFR−L bol relation could represent another crucial diagnostics to distinguish between the two AGN triggering modes, since the DI scenario predicts an appreciably lower scatter (especially at lowto-intermediate AGN luminosities) of the relation than the IT scenario. vi) Disk instabilities are unable to account for the observed fraction of AGN in groups for z < ∼ 1 and clusters for z < ∼ 0.7, while the IT scenario matches observational data well.

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A comprehensive study of large-scale structures in the GOODS-SOUTH field up to ${\mathsf z} \sim $ 2.5

Cited by 47 publications

References 72 publications

Physical and morphological properties ofz~ 3 Lyman break galaxies: dependence on Lyαline emission

Physical and morphological properties ofz~ 3 Lyman break galaxies: dependence on Lyαline emission

Galaxy Environment in the 3D-HST Fields: Witnessing the Onset of Satellite Quenching at z ∼ 1–2

Physical properties of AGN host galaxies as a probe of supermassive black hole feeding mechanisms

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