The great observatories origins deep survey

Abstract. We present new improved constraints on the Hubble parameter H(z) in the redshift range 0.15 < z < 1.1, obtained from the differential spectroscopic evolution of early-type galaxies as a function of redshift. We extract a large sample of early-type galaxies (∼ 11000) from several spectroscopic surveys, spanning almost 8 billion years of cosmic lookback time (0.15 < z < 1.42). We select the most massive, red elliptical galaxies, passively evolving and without signature of ongoing star formation. Those galaxies can be used as standard cosmic chronometers, as firstly proposed by Jimenez & Loeb (2002), whose differential age evolution as a function of cosmic time directly probesWe analyze the 4000Å break (D4000) as a function of redshift, use stellar population synthesis models to theoretically calibrate the dependence of the differential age evolution on the differential D4000, and estimate the Hubble parameter taking into account both statistical and systematical errors.We provide 8 new measurements of H(z) (see Tab. 4), and determine its change in H(z) to a precision of 5 − 12% mapping homogeneously the redshift range up to z ∼ 1.1; for the first time, we place a constraint on H(z) at z = 0 with a precision comparable with the one achieved for the Hubble constant (about 5-6% at z ∼ 0.2), and covered a redshift range (0.5 < z < 0.8) which is crucial to distinguish many different quintessence cosmologies.These measurements have been tested to best match a ΛCDM model, clearly providing a statistically robust indication that the Universe is undergoing an accelerated expansion. This method shows the potentiality to open a new avenue in constrain a variety of alternative cosmologies, especially when future surveys (e.g. Euclid) will open the possibility to extend it up to z ∼ 2.-1 -

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“…[44]). The spectra have been obtained from VVDS [45], VIMOS [46], and FORS2 [43,47]. Mass estimates have been taken from Ref.…”

Section: Goods-s Samplementioning

confidence: 99%

“…Old passive ETGs were extracted from the GOODS-S field [43] combining morphological and photometric criteria based on optical color cuts as a function of redshift (for more details on the sample selection, see Ref. [44]).…”

Section: Goods-s Samplementioning

confidence: 99%

Improved constraints on the expansion rate of the Universe up to z ∼ 1.1 from the spectroscopic evolution of cosmic chronometers

Moresco

Cimatti

Jiménez

et al. 2012

J. Cosmol. Astropart. Phys.

682

361

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“…When a spectroscopic redshift is present, the relative source catalog is reported, as follows: (1) CXO-CDFS (S04); (2) K20 (Mignoli et al 2005); (3) GOODS (Vanzella et al 2005(Vanzella et al , 2006(Vanzella et al , 2008Popesso et al 2008); (4) COMBO-17 (Wolf et al 2003); (5) VVDS (Le Fevre et al 2004); (6) other Cristiani et al 2000). Otherwise, the redshift is from SED fitting ) and is reported with its 1σ confidence interval.…”

Section: Optical+infrared Photometry and Photometric Redshiftsmentioning

confidence: 99%

Black hole growth and starburst activity atz= 0.6–4 in the Chandra Deep Field South

Brusa¹,

Fiore

Santini

et al. 2009

A&A

Self Cite

102

113

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Aims. The co-evolution of host galaxies and the active black holes which reside in their centre is one of the most important topics in modern observational cosmology. Here we present a study of the properties of obscured active galactic nuclei (AGN) detected in the CDFS 1 Ms observation and their host galaxies. Methods. We limited the analysis to the MUSIC area, for which deep K-band observations obtained with ISAAC@VLT are available, ensuring accurate identifications of the counterparts of the X-ray sources as well as reliable determination of photometric redshifts and galaxy parameters, such as stellar masses and star formation rates. In particular, we: 1) refined the X-ray/infrared/optical association of 179 sources in the MUSIC area detected in the Chandra observation; 2) studied the host galaxies observed and rest frame colors and properties. Results. We found that X-ray selected (L X > ∼ 10 42 erg s −1 ) AGN show Spitzer colors consistent with both AGN and starburst dominated infrared continuum; the latter would not have been selected as AGN from infrared diagnostics. The host galaxies of X-ray selected obscured AGN are all massive (M * > 10 10 M ) and, in 50% of the cases, are also actively forming stars (1/SSFR < t Hubble ) in dusty environments. The median L/L Edd value of the active nucleus is between 2% and 10% depending on the assumed M BH /M * ratio. Finally, we found that the X-ray selected AGN fraction increases with the stellar mass up to a value of ∼30% at z > 1 and M * > 3 × 10 11 M , a fraction significantly higher than in the local Universe for AGN of similar luminosities.

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“…Photometric redshifts were estimated using GAaP magnitudes with BPZ, following Hildebrandt et al (2012). Kuijken et al (2015) compared the photometric redshifts to ∼17 000 spectroscopic redshifts in the zCOSMOS (Lilly et al 2007) and ESO/GOODS (Vanzella et al 2008;Balestra et al 2010) surveys. They found that the peak of the posterior distribution, z B , is biased by less than 2 per cent in the range 0.005 < z B < 1.0.…”

Section: Photometric Redshiftsmentioning

confidence: 99%

The masses of satellites in GAMA galaxy groups from 100 square degrees of KiDS weak lensing data

Sifón¹,

Cacciato²,

Hoekstra³

et al. 2015

Mon. Not. R. Astron. Soc.

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We use the first 100 deg 2 of overlap between the Kilo-Degree Survey (KiDS) and the Galaxy And Mass Assembly (GAMA) survey to determine the galaxy halo mass of ∼10,000 spectroscopically-confirmed satellite galaxies in massive (M > 10 13 h −1 M ) galaxy groups. Separating the sample as a function of projected distance to the group centre, we jointly model the satellites and their host groups with Navarro-Frenk-White (NFW) density profiles, fully accounting for the data covariance. The probed satellite galaxies in these groups have total masses log M sub /(h −1 M ) ≈ 11.7 − 12.2 consistent across group-centric distance within the errorbars. Given their typical stellar masses, log M ,sat /(h −2 M ) ∼ 10.5, such total masses imply stellar mass fractions of M ,sat /M sub ≈ 0.04 h −1 . The average subhalo hosting these satellite galaxies has a mass M sub ∼ 0.015M host independent of host halo mass, in broad agreement with the expectations of structure formation in a ΛCDM universe.

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The great observatories origins deep survey

Cited by 333 publications

References 42 publications

Improved constraints on the expansion rate of the Universe up to z ∼ 1.1 from the spectroscopic evolution of cosmic chronometers

Improved constraints on the expansion rate of the Universe up to z ∼ 1.1 from the spectroscopic evolution of cosmic chronometers

Black hole growth and starburst activity atz= 0.6–4 in the Chandra Deep Field South

The masses of satellites in GAMA galaxy groups from 100 square degrees of KiDS weak lensing data

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