The Gemini Deep Deep Survey. I. Introduction to the Survey, Catalogs, and Composite Spectra

Abraham, Roberto; Glazebrook, Karl; McCarthy, Patrick J.; Crampton, D.; Murowinski, Richard; Jørgensen, Inger; Roth, Kathy; Hook, I. M.; Savaglio, S.; Chen, Hsiao‐Wen; Marzke, Ronald O.; Carlberg, R. G.

doi:10.1086/383557

Cited by 259 publications

(299 citation statements)

References 34 publications

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“…4. For comparison, we also show the composite spectrum of field early-type galaxies at a similar redshift and covering are similar range of stellar masses, which was obtained by combining 11 GDSS (Abraham et al 2004) and 3 GMASS (Cimatti et al 2008) spectra in the range 1.3 < z < 1.5. It is interesting to note that, similar to what was found by Gobat et al (2008) (see also Rettura et al 2008), who compared the SFHs of earlytype galaxies in a massive cluster at z = 1.24 with those in the field, the 4000 Å break in cluster early-type galaxies appears to be larger than those in field galaxies, suggesting a higher formation redshift or a shorter duration of the star forming phase for early-type galaxies in massive clusters.…”

Section: Figmentioning

confidence: 99%

Multi-wavelength study of XMMU J2235.3-2557: the most massive galaxy cluster at z > 1

Rosati¹,

Tozzi

Gobat

et al. 2009

A&A

138

187

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Context. The galaxy cluster XMMU J2235.3−2557 (hereafter XMM2235), spectroscopically confirmed at z = 1.39, is one of the most distant X-ray selected galaxy clusters. It has been at the center of a multi-wavelength observing campaign with ground and space facilities. Aims. We characterize the galaxy populations of passive members, the thermodynamical properties and metal abundance of the hot gas, and the total mass of the system using imaging data with HST/ACS (i 775 and z 850 bands) and VLT/ISAAC (J and K S bands), extensive spectroscopic data obtained with VLT/FORS2, and deep (196 ks) Chandra observations. Methods. Chandra data allow temperature and metallicity to be measured with good accuracy and the X-ray surface brightness profile to be traced out to 1 (or 500 kpc), thus allowing the mass to be reliably estimated. Out of a total sample of 34 spectroscopically confirmed cluster members, we selected 16 passive galaxies (without detectable [OII]) within the central 2 (or 1 Mpc) with ACS coverage, and inferred star formation histories for subsamples of galaxies inside and outside the core by modeling their spectrophotometric data with spectral synthesis models. Results. Chandra data show a regular elongated morphology, closely resembling the distribution of core galaxies, with a significant cool core. We measure a global X-ray temperature of kT = 8.6 +1.3 −1.2 keV (68% confidence), which we find to be robust against several systematics involved in the X-ray spectral analysis. By detecting the rest frame 6.7 keV Iron K line in the Chandra spectrum, we measure a metallicity Z = 0.26 +0.20 −0.16 Z . In the likely hypothesis of hydrostatic equilibrium, we obtain a total mass of M tot (< 1 Mpc) = (5.9 ± 1.3) × 10 14 M . By modeling both the composite spectral energy distributions and spectra of the passive galaxies in and outside the core, we find a strong mean age radial gradient. Core galaxies, with stellar masses in excess of 10 11 M , appear to have formed at an earlier epoch with a relatively short star formation phase (z = 5−6), whereas passive galaxies outside the core show spectral signatures suggesting a prolonged star formation phase to redshifts as low as z ≈ 2. Conclusions. Overall, our analysis implies that XMM2235 is the hottest and most massive bona-fide cluster discovered to date at z > 1, with a baryonic content, both its galaxy population and intracluster gas, in a significantly advanced evolutionary stage at 1/3 of the current age of the Universe.

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Section: Figmentioning

confidence: 99%

Multi-wavelength study of XMMU J2235.3-2557: the most massive galaxy cluster at z > 1

Rosati¹,

Tozzi

Gobat

et al. 2009

A&A

138

187

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“…Of these 108 objects, 66 galaxies were selected from the (mostly) I-limited spectroscopic catalogue of the FORS deep field (FDF) spectroscopic survey (Noll et al 2004) and originally inspected for z > 2 by NP05. In addition, 34 galaxies were taken from the K s < 20-selected K20 survey in the GOODS-S and a field around quasar 0055-2659 (Cimatti et al 2002;Mignoli et al 2005), and 8 galaxies were selected from the I-and K s -limited Gemini deep deep survey (GDDS, Abraham et al 2004). For 88 objects from the FDF and K20 samples, the UV continuum slope could be determined in addition to the presence/absence of the UV bump (see NPPS).…”

Section: The Fdf K20 and Gdds Samplesmentioning

confidence: 99%

GMASS ultradeep spectroscopy of galaxies at z ~ 2

Noll

Pierini

Cimatti

et al. 2009

A&A

112

175

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Aims. The properties of dust attenuation at rest-frame UV wavelengths are inferred from very high-quality FORS 2 spectra of 78 galaxies from the GMASS survey at redshift 1 < z < 2.5. These objects complement a previously investigated sample of 108 UV-luminous, intermediate-mass (i.e., with stellar masses ∼10 10 −10 11 M ) galaxies at similar redshifts, selected from the FDF spectroscopic survey, the K20 survey, and the GDDS. Detection of the broad absorption feature centred on about 2175 Å ("UV bump") implies that the average UV extinction curve of a galaxy more closely resembles that of the Milky Way (MW) or the Large Magellanic Cloud (LMC), and differs from that of the Small Magellanic Cloud (SMC). Methods. The shape of the UV extinction curve is constrained by a parametric description of the rest-frame UV continuum with the support of a suite of models combining radiative transfer and stellar population synthesis. The UV bump is further characterised by fitting Lorentzian-like profiles. Results. Spectra exhibit a significant 2175 Å feature in at least 30% of the cases, especially those suffering from substantial reddening. If attenuation is dominated by dust ejected from the galaxy main body via galactic winds or more localised superwinds, UV extinction curves in-between those of the SMC and LMC characterise UV-luminous, intermediate-mass galaxies at 1 < z < 2.5. The fraction of galaxies with extinction curves differing from the SMC one increases, if more dust resides in the galactic plane or dust attenuation depends on stellar age. On average, the width of the manifested UV bumps is about 60% of the values typically measured along sightlines in the LMC and MW. This suggests the presence of dust similar to that found in the "supergiant" shell of ionised filaments LMC 2, close to 30 Dor. The presence of the carriers of the UV bump (probably organic carbon and amorphous silicates) at 1 < z < 2.5 argues for outflows from asymptotic giant branch (AGB) stars being copious then. Consistent with their higher star-formation rates, the GMASS galaxies with a manifested UV bump are more luminous at rest-frame 8 μm, where the emission is dominated by polycyclic aromatic hydrocarbons (also products of AGB stars). In addition, they exhibit larger equivalent widths for prominent UV (metal) absorption features, mostly of interstellar origin, which indicates overall more evolved stellar populations. Conclusions. We conclude that diversification of the small-size dust component (responsible for the differential extinction at UV wavelengths and the emission at mid-IR wavelengths) has already started in the most evolved star-forming systems at 1 < z < 2.5.

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“…Moreover, compared with other observational data, it is more rewarding to investigate the observational H(z) data directly, because it can take the fine structure of H(z) into consideration and then use the important information that this structure provides. By using the differential ages of passively evolving galaxies determined from the Gemini Deep Deep Survey (GDDS) (Abraham et al 2004) and archival data (Treu et al 2001(Treu et al , 2002Nolan et al 2003a,b), Simon et al (2005) determined nine values of the Hubble parameter H(z) in the range 0 ≤ z ≤ 1.8, which have been used to constrain the parameters of various dark energy models (Samushia & Ratra 2006;Wei & Zhang 2007;Wu & Yu 2007a,b;Zhang & Zhu 2007;Kurek & Szydlowski 2007;Lazkoz & Majerotto 2007;Sen & Scherrer 2008;Wan et al 2007;Xu et al 2008;Zhai et al 2010). The H(z) data at 11 different redshifts were determined from the differential ages of red-envelope galaxies (Stern et al 2010), and two more Hubble parameter data points H(z = 0.24) = 79.69 ± 4.61 and H(z = 0.43) = 86.45 ± 5.96 were obtained by Gaztañaga et al (2009) from observations of BAO peaks (for a review of the observational H(z) data, see Zhang et al 2010).…”

Section: The Observational H(z) Datamentioning

confidence: 99%

Observational constraints on interacting dark matter model without dark energy

Cao

Zhu

Liang

2011

A&A

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Aims. The interacting dark matter (IDM) scenario allows for the acceleration of the Universe without dark energy. Methods. We constrain the IDM model by using the newly revised observational data including H(z) data and Union2 SNe Ia via the Markov chain Monte Carlo method. Results. When mimicking the ΛCDM model, we obtain a more stringent upper limit to the effective annihilation term at κC 1 ≈ 10 −3.4 Gyr −1 , and a tighter lower limit to the relevant mass of dark matter particles at M x ≈ 10 −8.6 Gev. When mimicking the wCDM model, we find that the effective equation of state of IDM is consistent with the concordance ΛCDM model and appears to be most consistent with the effective phantom model with a constant EoS for which w < −1.

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The Gemini Deep Deep Survey. I. Introduction to the Survey, Catalogs, and Composite Spectra

Cited by 259 publications

References 34 publications

Multi-wavelength study of XMMU J2235.3-2557: the most massive galaxy cluster at z > 1

Multi-wavelength study of XMMU J2235.3-2557: the most massive galaxy cluster at z > 1

GMASS ultradeep spectroscopy of galaxies at z ~ 2

Observational constraints on interacting dark matter model without dark energy

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