The evolution of the luminosity functions in the FORS Deep Field from low to high redshift

Gabasch, A.; Bender, Ralf; Seitz, S.; Hopp, U.; Saglia, R.; Feulner, Georg; Snigula, J.; Drory, Niv; Appenzeller, I.; Heidt, J.; Mehlert, D.; Noll, Stefan; Böhm, A.; Jäger, Klaus; Ziegler, B.; Fricke, K. J.

doi:10.1051/0004-6361:20035909

Cited by 154 publications

(282 citation statements)

References 113 publications

(243 reference statements)

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“…One sample is selected in luminosity, M B −20 (∼M * B at z ∼ 0; Faber et al 2007), which comprises 1122 sources. The value of M * B is 1 mag brighter at z ∼ 1 than locally (Gabasch et al 2004;Ilbert et al 2005;Faber et al 2007), evolution that reflects the descent in the star formation rate density of the universe since z ∼ 1 (e.g., Hopkins & Beacom 2006). Hence, if we assume a constant M B 7 http://www.stsci.edu/science/goods/ 8 http://archive.stsci.edu/prepds/goods/ 9 http://guaix.fis.ucm.es/∼pgperez/Proyectos/ucmcsdatabase.en.html cut, we select different areas of the luminosity function at each redshift, biasing our results.…”

Section: Galaxy Samplesmentioning

confidence: 78%

THE MINOR ROLE OF GAS-RICH MAJOR MERGERS IN THE RISE OF INTERMEDIATE-MASS EARLY TYPES ATz⩽ 1

López-Sanjuan

Balcells

Pérez‐González

et al. 2010

ApJ

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We study the evolution of galaxy structure since z ∼ 1 to the present. From a Great Observatories Origins Deep Survey South (GOODS-S) multi-band catalog, we define (blue) luminosity-and mass-weighted samples, limited by M B −20 and M 10 10 M , comprising 1122 and 987 galaxies, respectively. We extract early-type (ET; E/S0/ Sa) and late-type (LT; Sb-Irr) subsamples by their position in the concentration-asymmetry plane, in which galaxies exhibit a clear bimodality. We find that the ET fraction, f ET , rises with cosmic time, with a corresponding decrease in the LT fraction, f LT , in both luminosity-and mass-selected samples. However, the evolution of the comoving number density is very different: the decrease in the total number density of M B −20 galaxies since z = 1 is due to the decrease in the LT population, which accounts for ∼75% of the total star formation rate in the range under study, while the increase in the total number density of M 10 10 M galaxies in the same redshift range is due to the evolution of ETs. This suggests that we need a structural transformation between LT galaxies that form stars actively and ET galaxies in which the stellar mass is located. Comparing the observed evolution with the gas-rich major merger rate in GOODS-S, we infer that only ∼20% of the new ET galaxies with M 10 10 M appeared since z ∼ 1 can be explained by this kind of mergers, suggesting that minor mergers and secular processes may be the driving mechanisms of the structural evolution of intermediate-mass (M ∼ 4 × 10 10 M ) galaxies since z ∼ 1.

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Section: Galaxy Samplesmentioning

confidence: 78%

THE MINOR ROLE OF GAS-RICH MAJOR MERGERS IN THE RISE OF INTERMEDIATE-MASS EARLY TYPES ATz⩽ 1

López-Sanjuan

Balcells

Pérez‐González

et al. 2010

ApJ

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“…Below this, VVDS claims to see a steepening in faint-end slope from $ À1:2 at z ¼ 0:05 to $ À1:5 at z ¼ 1. Neither DEEP2 nor COMBO-17 goes deep enough to test this, but, as noted in x 1, Gabasch et al (2004;FDF) go 2.5 mag fainter and do not see it, getting ¼ À1:25 at all redshifts. Relative to the local Schechter function, the All data brighten back in time (M Ã B ) but stay roughly constant in number density ( Ã ).…”

Section: The Deep and Combo-17 Luminosity Functionsmentioning

confidence: 93%

“…In spite of lower precision, photometric redshifts yield a larger number of redshifts per unit telescope time and enable distances to be measured for galaxies that are too faint for spectroscopy. This approach has been pursued using both spacebased (e.g., Takeuchi et al 2000;Poli et al 2001;Bolzonella et al 2002) and ground-based data (e.g., Fried et al 2001;Drory et al 2003;Wolf et al 2003, hereafter W03;Chen et al 2003;Gabasch et al 2004). Of the photometric redshift surveys, the ones most comparable to the present work are and the FORS Deep Field (FDF; Gabasch et al 2004).…”

Section: Introductionmentioning

confidence: 95%

“…This approach has been pursued using both spacebased (e.g., Takeuchi et al 2000;Poli et al 2001;Bolzonella et al 2002) and ground-based data (e.g., Fried et al 2001;Drory et al 2003;Wolf et al 2003, hereafter W03;Chen et al 2003;Gabasch et al 2004). Of the photometric redshift surveys, the ones most comparable to the present work are and the FORS Deep Field (FDF; Gabasch et al 2004). The latter used a sample of more than 5500 galaxies down to I AB ¼ 26:8 to measure the total rest-frame B-band luminosity function from z $ 0:4 to $4.…”

Section: Introductionmentioning

confidence: 99%

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Galaxy Luminosity Functions toz∼1 from DEEP2 and COMBO‐17: Implications for Red Galaxy Formation

Faber

Willmer

Wolf

et al. 2007

ApJ

989

1,031

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The DEEP2 and COMBO-17 surveys are compared to study luminosity functions of red and blue galaxies to z $ 1. The two surveys have different methods and sensitivities, but nevertheless results agree. After z $ 1, M Ã B has dimmed by 1.2Y1.3 mag for all colors of galaxies, Ã for blue galaxies has hardly changed, and Ã for red galaxies has at least doubled (our formal value is $0.5 dex). Luminosity density j B has fallen by 0.6 dex for blue galaxies but has remained nearly constant for red galaxies. These results imply that the number and total stellar mass of blue galaxies have been substantially constant since z $ 1, whereas those of red galaxies (near L Ã ) have been significantly rising. To explain the new red galaxies, a ''mixed'' scenario is proposed in which star formation in blue cloud galaxies is quenched, causing them to migrate to the red sequence, where they merge further in a small number of stellar mergers. This mixed scenario matches the local boxy-disky transition for nearby ellipticals, as well as red sequence stellar population scaling laws such as the color-magnitude and Mg-relations (which are explained as fossil relics from blue progenitors). Blue galaxies enter the red sequence via different quenching modes, each of which peaks at a different characteristic mass and time. The red sequence therefore likely builds up in different ways at different times and masses, and the concept of a single process that is ''downsizing'' (or upsizing) probably does not apply. Our claim in this paper of a rise in the number of red galaxies applies to galaxies near L Ã . Accurate counts of brighter galaxies on the steep part of the Schechter function require more accurate photometry than is currently available.

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“…No other nearby objects are found at the 3σ significance level (corresponding to 0.03 L * ). At z = 2 a luminous L * galaxy has an absolute magnitude of U * AB = −21.9 mag (Gabasch et al 2004), and an observed magnitude of U AB = 24.0 mag in the adopted cosmology. The numbered objects in Fig.…”

Section: Nearby Galaxies and Coloursmentioning

confidence: 98%

Uncovering strong MgII absorbing galaxies

Christensen

Noterdaeme

Petitjean

et al. 2009

A&A

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Context. The nature of the galaxies that give rise to absorption lines, such as damped Lyman-α systems (DLAs) or strong Mg ii lines, in quasar spectra is difficult to investigate in emission. These galaxies can be very faint and located close to the lines of sight of the much brighter background quasars. Aims. Taking advantage of the total absorption of the QSO light bluewards of the Lyman limit of two DLAs at z > 3.4, we look for the continuum emission from intervening galaxies at z ≈ 2 that are identified via strong metal absorption lines. The Mg ii absorbers have equivalent width large enough to be potential DLA systems. Methods. Deep images are obtained with the FOcal Reducer and Spectrograph (FORS1) on the Very Large Telescope for the fields towards SDSS J110855+120953 and SDSS J140850+020522. These quasars have Mg ii absorption lines at z = 1.87 (W r (Mg ii) = 2.46 Å) and z = 1.98 (W r (Mg ii) = 1.89 Å), respectively, and each QSO has two intervening higher redshift DLAs at z > 3. The U and R bands of FORS1 lie blue and redwards of the Lyman limit of the background DLAs, allowing us to search for emission from the foreground galaxies directly along the lines of sight to the QSOs. Results. No galaxies are found close to the sight line of the QSO to a point source limit of U AB ∼ 28.0. In both fields, the closest objects lie at an impact parameter of ∼5 corresponding to ∼40 kpc in projection at z = 2, and have typical colours of star forming galaxies at that redshift. However, the currently available data do not allow us to confirm if the galaxies lie at the same redshifts as the absorption systems. A more extended structure is visible in the SDSS J14085+020522 field at an impact parameter of 0. 8 or 7 kpc. If these objects are at z ≈ 2 their luminosities are 0.03-0.04 L * in both fields. The star formation rates estimated from the UV flux are 0.5-0.6 M yr −1 , while the SFRs are half these values if the U band flux is due to Lyα emission alone. Conclusions. The non-detection of galaxies near to the line of sight is most likely explained by low metallicities and luminosities of the Mg ii galaxies. Alternatively, the Mg ii clouds are part of extended halos or in outflows from low-metallicity galaxies.

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The evolution of the luminosity functions in the FORS Deep Field from low to high redshift

Cited by 154 publications

References 113 publications

THE MINOR ROLE OF GAS-RICH MAJOR MERGERS IN THE RISE OF INTERMEDIATE-MASS EARLY TYPES ATz⩽ 1

THE MINOR ROLE OF GAS-RICH MAJOR MERGERS IN THE RISE OF INTERMEDIATE-MASS EARLY TYPES ATz⩽ 1

Galaxy Luminosity Functions toz∼1 from DEEP2 and COMBO‐17: Implications for Red Galaxy Formation

Uncovering strong MgII absorbing galaxies

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