The z=2.72 galaxy cB58: a gravitational fold arc lensed by the cluster MS 1512+36

Seitz, S.; Saglia, R.; Bender, Ralf; Hopp, U.; Belloni, P.; Ziegler, B.

doi:10.1046/j.1365-8711.1998.01443.x

Cited by 79 publications

(99 citation statements)

References 27 publications

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“…Conditions were mostly photometric during both Keck runs, and the typical seeing in the K band was FWHM. 0A .5È0A .6 Ellingson et al 1996) have been corrected for the gravitational magniÐcation by a factor of 30 derived by Seitz et al 1998. h NIRSPEC N4 band spans the wavelength range 1.3È1.6 km.…”

Section: Data Acquisitionmentioning

confidence: 99%

The Rest‐Frame Optical Spectra of Lyman Break Galaxies: Star Formation, Extinction, Abundances, and Kinematics

Pettini

Shapley

Steidel

et al. 2001

ApJ

742

972

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We present the Ðrst results of a spectroscopic survey of Lyman break galaxies (LBGs) in the nearinfrared aimed at detecting the emission lines of [O II], [O III], and Hb from the H II regions of normal star-forming galaxies at z^3. From observations of 15 objects with the Keck telescope and the Very Large Telescope augmented with data from the literature for an additional four objects, we reach the following main conclusions. The rest-frame optical properties of LBGs at the bright end of the luminosity function are remarkably uniform, their spectra are dominated by emission lines, [O III] is always stronger than Hb and [O II], and projected velocity dispersions are between 50 and 115 km s~1. Contrary to expectations, the star formation rates deduced from the Hb luminosity are on average no larger than those implied by the stellar continuum at 1500 presumably any di †erential extinction between A ; rest-frame optical and UV wavelengths is small compared to the relative uncertainties in the calibrations of these two star formation tracers. For the galaxies in our sample, the abundance of oxygen can only be determined to within 1 order of magnitude without recourse to other emission lines ([N II] and Ha), which are generally not available. Even so, it seems well established that LBGs are the most metalenriched structures at z^3, apart from quasi-stellar objects, with abundances greater than about 1/10 solar and generally higher than those of damped Lya systems at the same epoch. They are also signiÐ-cantly overluminous for their metallicities ; this is probably an indication that their mass-to-light ratios are low compared to present-day galaxies. At face value, the measured velocity dispersions imply virial masses of about 1010 within half-light radii of 2.5 kpc. The corresponding mass-to-light ratios, M _ M/L B 0.15 in solar units, are indicative of stellar populations with ages between 108 and 109 yr, consistent with the UV-optical spectral energy distributions. However, we are unable to establish conclusively whether or not the widths of the emission lines reÑect the motions of the H II regions within the gravitational potential of the galaxies, even though in two cases we see hints of rotation curves. All 19 LBGs observed show evidence for galactic-scale superwinds ; such outÑows have important consequences for regulating star formation, distributing metals over large volumes, and allowing Lyman continuum photons to escape and ionize the intergalactic medium.

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Section: Data Acquisitionmentioning

confidence: 99%

The Rest‐Frame Optical Spectra of Lyman Break Galaxies: Star Formation, Extinction, Abundances, and Kinematics

Pettini

Shapley

Steidel

et al. 2001

ApJ

742

972

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“…Owing to its gravitationally lensed nature, MS 1512-cB58 is one of the brightest known LBGs. This object is at z ∼ 2.73 and has a luminous mass of ∼10 10 M , a star formation rate ψ(t sf ) ∼ 40 M yr −1 (Pettini et al 2002) and an effective radius of r L ∼ 2 kpc (Seitz et al 1998), for a Ω m = 0.3, Ω Λ = 0.7, h = 0.70 cosmology. Pettini et al (2002) concluded that the abundances of O, Mg and Si are ∼2/5 of their solar values, whereas [Fe/H] = -1.15, hence underabundant by a further factor of >3 with respect to the other elements.…”

Section: Lyman Break Galaxiesmentioning

confidence: 99%

The chemical evolution of elliptical galaxies with stellar and QSO dust production

Pipino

Fan

Matteuccí

et al. 2010

A&A

145

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Context. The presence of dust strongly affects the way we see galaxies and also the chemical abundances we measure in gas. It is therefore important to study the chemical evolution of galaxies by taking into account dust evolution. Aims. We aim at performing a detailed study of abundance ratios of high redshift objects and their dust properties. We focus on Lyman-Break galaxies (LBGs) and Quasar (QSO) hosts as likely progenitors of low-and high-mass present-day elliptical galaxies, respectively. Methods. We have adopted a chemical evolution model for elliptical galaxies taking into account the dust production from low and intermediate mass stars, supernovae Ia, supernovae II, QSOs and both dust destruction and accretion processes. By means of such a model we have followed the chemical evolution of ellipticals of different baryonic masses. Our model complies with chemical downsizing.Results. We made predictions for the abundance ratios versus metallicity trends for models of differing masses that can be used to constrain the star formation rate, initial mass function and dust mass in observed galaxies. We predict the existence of a high redshift dust mass-stellar mass relationship. We have found a good agreement with the properties of LBGs if we assume that they formed at redshift z = 2-4. In particular, a non-negligible amount of dust is needed to explain the observed abundance pattern. We studied the QSO SDSS J114816, one of the most distant QSO ever observed (z = 6.4), and we have been able to reproduce the amount of dust measured in this object. The dust is clearly due to the production from supernovae and the most massive AGB stars as well as from the grain growth in the interstellar medium. The QSO dust is likely to dominate only in the very central regions of the galaxies and during the early development of the galactic wind.

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“…Assuming for an Im-type SED ( Seitz et al 1998, who give R \ 23.9 and after demagniÐcation. Applying a distance K AB \ 23.0 modulus of 46.8 mag, a K-correction bandpass term of 1.4 mag, and assuming B[V \ 0.27 for an Im-type spectral energy distribution (Fukugita et al 1995) yields the Ðnal rest-frame B magnitude of [22.1.…”

Section: Evolution Of Chemical Propertiesmentioning

confidence: 99%

Near‐Infrared Spectroscopy of Two Galaxies atz = 2.3 andz = 2.9: New Probes of Chemical and Dynamical Evolution at High Redshift

Kobulnicky

Koo

2000

ApJ

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This study presents Keck optical and infrared spectroscopy of the rest-frame ultraviolet and optical emission lines in two Lya-emitting galaxies at z [ 2. These data provide insight on the evolution of fundamental galaxy scaling relations at early epochs, especially the luminosity-velocity and luminositymetallicity relations. Spectral diagnostics suggest that the Coup galaxy at z \ 2.3 and Lynx Fourre 2-9691, a serendipitously discovered, luminous Lyman drop galaxy at z \ 2.9, are star-forming galaxies without active nuclei. Lynx 2-9691 exhibits extended [O III] emission over a diameter of greater than 28 kpc, reminiscent of the Lya nebulae discovered near Lyman drop galaxies. We estimate star formation rates of 59 and 111 yr~1, respectively, from Balmer recombination line luminosities, 2È3 times M _ higher than inferred from the ultraviolet continuum. The ratios of strong nebular emission lines indicate subsolar oxygen abundances in the range 8.Interestingly, Z _ ). Galactic metal-rich globular clusters have similar metallicities, consistent with the idea that we could be seeing the formation of galaxies like the Milky Way at z D 3. The measured gas-phase oxygen abundances are greater than 4È10 times higher than the Z \ 0.1 metallicities found in damped Lya (DLA) Z _ absorbers at similar redshifts, indicating that DLA systems trace fundamentally di †erent environments than the vigorously star-forming objects observed here. If this intense star formation activity represents the dominant formation episodes for stars in todayÏs spiral bulges or ellipticals, then the evolved descendants in the local universe should exhibit similarly subsolar metallicities in their dominant stellar populations that formed 8È10 Gyr ago. When these new data are combined with a sample of four other high-redshift spectroscopic results from the literature, we Ðnd that star-forming galaxies at z D 3 are 2È4 mag more luminous than local spiral galaxies of similar metallicity and thus are o †set from the local luminosity-metallicity relation. Their kinematic line widths are km s~1, making this sample p v \ 65È130 1È3 mag more luminous than local galaxies of similar line width and mass. Less luminous Lyman drop galaxies need to be studied to see if these deviations are universal or apply to only the most luminous high-redshift galaxies.

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The z=2.72 galaxy cB58: a gravitational fold arc lensed by the cluster MS 1512+36

Cited by 79 publications

References 27 publications

The Rest‐Frame Optical Spectra of Lyman Break Galaxies: Star Formation, Extinction, Abundances, and Kinematics

The Rest‐Frame Optical Spectra of Lyman Break Galaxies: Star Formation, Extinction, Abundances, and Kinematics

The chemical evolution of elliptical galaxies with stellar and QSO dust production

Near‐Infrared Spectroscopy of Two Galaxies atz = 2.3 andz = 2.9: New Probes of Chemical and Dynamical Evolution at High Redshift

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