The FORS Deep Field: Field selection, photometric observations and photometric catalog

Heidt, J.; Appenzeller, I.; Gabasch, A.; Jaeger, Klaus; Seitz, S.; Bender, Ralf; Boehm, A.; Snigula, J.; Fricke, K. J.; Hopp, U.; Kuemmel, M.; Moellenhoff, C.; Szeifert, T.; Ziegler, B.; Drory, Niv; Mehlert, D.; Moorwood, A. F. M.; Nicklas, H.; Noll, Stefan; Saglia, R.; Seifert, W.; Stahl, O.; Sutorius, Eckhard; Wagner, S. J.

doi:10.1051/0004-6361:20021620

Cited by 82 publications

(105 citation statements)

References 34 publications

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“…To select our spectroscopic targets, we relied on two multiband photometric surveys: the FORS Deep Field (FDF; Heidt et al 2003) and the William Herschel Deep Field (WHDF; Metcalfe et al 2001). These comprise deep imaging in the filters U, B, g, R, I, J, K (FDF) and U, B, R, I, H, K (WHDF).…”

Section: Sample Selection and Observationsmentioning

confidence: 99%

Disk galaxy scaling relations at intermediate redshifts

Boehm¹,

Ziegler²

2016

A&A

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Aims. Galaxy scaling relations such as the Tully-Fisher relation (between the maximum rotation velocity V max and luminosity) and the velocity-size relation (between V max and the disk scale length) are powerful tools to quantify the evolution of disk galaxies with cosmic time. Methods. We took spatially resolved slit spectra of 261 field disk galaxies at redshifts up to z ≈ 1 using the FORS instruments of the ESO Very Large Telescope. The targets were selected from the FORS Deep Field and William Herschel Deep Field. Our spectroscopy was complemented with HST/ACS imaging in the F814W filter. We analyzed the ionized gas kinematics by extracting rotation curves from the two-dimensional spectra. Taking into account all geometrical, observational, and instrumental effects, these rotation curves were used to derive the intrinsic V max .Results. Neglecting galaxies with disturbed kinematics or insufficient spatial rotation curve extent, V max was reliably determined for 124 galaxies covering redshifts 0.05 < z < 0.97. This is one of the largest kinematic samples of distant disk galaxies to date. We compared this data set to the local B-band Tully-Fisher relation and the local velocity-size relation. The scatter in both scaling relations is a factor of ∼2 larger at z ≈ 0.5 than at z ≈ 0. The deviations of individual distant galaxies from the local Tully-Fisher relation are systematic in the sense that the galaxies are increasingly overluminous toward higher redshifts, corresponding to an overluminosity ∆M B = −(1.2 ± 0.5) mag at z = 1. This luminosity evolution at given V max is probably driven by younger stellar populations of distant galaxies with respect to their local counterparts, potentially combined with modest changes in dark matter mass fractions. The analysis of the velocity-size relation reveals that disk galaxies of a given V max have grown in size by a factor of ∼1.5 over the past ∼8 Gyr, most likely through accretion of cold gas and/or small satellites. From scrutinizing the combined evolution in luminosity and size, we find that the galaxies that show the strongest evolution toward smaller sizes at z ≈ 1 are not those that feature the strongest evolution in luminosity, and vice versa.

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Section: Sample Selection and Observationsmentioning

confidence: 99%

Disk galaxy scaling relations at intermediate redshifts

Boehm¹,

Ziegler²

2016

A&A

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“…Together with local galaxy templates (e.g., Coleman et al 1980;Mannucci et al 2001;Kinney et al 1996), we used a set of semi-empirical templates based on observations plus fitted SED models (Maraston 1998;Bruzual & Charlot 2003) of ∼300 galaxies in the FORS Deep Field (Heidt et al 2003) and Hubble Deep Field (Williams et al 1996), in order to better represent objects to higher redshifts. A different prior on the redshift distribution is assumed for different types of templates (e.g.…”

Section: Photometric Redshiftsmentioning

confidence: 99%

Cluster galaxies in XMMU J2235-2557: galaxy population properties in most massive environments atz ~ 1.4

Strazzullo

Rosati

Pannella

et al. 2010

A&A

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130

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We present a multi-wavelength study of galaxy populations in the core of the massive, X-ray luminous cluster XMMU J2235 at z = 1.39, based on high quality VLT and HST photometry at optical and near-infrared wavelengths. We derive luminosity functions in the z, H, and K s bands, approximately corresponding to restframe U, R and z band. These show a faint-end slope consistent with being flat, and a characteristic magnitude M * close to passive evolution predictions of M * of local massive clusters, with a formation redshift z > 2. The color−magnitude and color-mass diagrams show evidence of a tight red sequence (intrinsic scatter < ∼ 0.08) of massive galaxies already in place, with overall old stellar populations and generally early-type morphology. Beside the red colors, these massive (>6 × 10 10 M ) galaxies typically show early-type spectral features, and rest-frame far-UV emission consistent with very low star formation rates (SFR < 0.2 M yr −1 ). Star forming spectroscopic members, with SFR of up to ∼100 M /yr, are all located at clustercentric distances > ∼ 250 kpc, with the central cluster region already appearing effectively quenched. Most part of the cluster galaxies more massive than 6 × 10 10 M within the studied area do not appear to host significant levels of star formation. The high-mass end of the galaxy populations in the core of this cluster appears to be in a very advanced evolutionary stage, not only in terms of formation of the stellar populations, but also of the assembly of the stellar mass. The high-mass end of the galaxy stellar mass function is essentially already in place. The stellar mass fraction estimated within r 500 (∼1%, Kroupa IMF) is already similar to that of local massive clusters. On the other hand, surface brightness distribution modeling of the massive red sequence galaxies may suggest that their size is often smaller than expected based on the local stellar mass vs. size relation. An evolution of the stellar mass vs. size relation might imply that, in spite of the overall early assembly of these sources, their evolution is not complete, and processes like minor (and likely dry) merging might still shape the structural properties of these objects to resemble those of their local counterparts, without substantially affecting their stellar mass or host stellar populations. Nonetheless, a definite conclusion on the actual relevance of size evolution for the studied early-type sample is precluded by possible systematics and biases.

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“…The FDF (Heidt et al 2003) offers photometry in the U, B, g, R, I, 834 nm, z, J, and K bands and is complimented by deep spectroscopic observations (Noll et al 2004). In this Letter we use the I-selected subsample covering the deep central part Note.-The SSFR is given in units of Gyr Ϫ1 .…”

Section: The Galaxy Samplesmentioning

confidence: 99%

Specific Star Formation Rates to Redshift 5 from the FORS Deep Field and the GOODS-S Field

Feulner

Gabasch

Salvato

et al. 2005

ApJ

148

150

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We explore the buildup of stellar mass in galaxies over the wide redshift range by studying the 0.4 ! z ! 5.0 evolution of the specific star formation rate (SSFR), defined as the star formation rate per unit stellar mass, as a function of stellar mass and age. Our work is based on a combined sample of ∼9000 galaxies from the FORS Deep Field and the GOODS-S field, providing high statistical accuracy and relative insensitivity against cosmic variance. As at lower redshifts, we find that lower mass galaxies show higher SSFRs than higher mass galaxies, although highly obscured galaxies remain undetected in our sample. Furthermore, the highest mass galaxies contain the oldest stellar populations at all redshifts, in principle agreement with the existence of evolved, massive galaxies at . It is remarkable, however, that this trend continues to very high redshifts of . We also 1 ! z ! 3 z ∼ 4 show that with increasing redshift, the SSFR for massive galaxies increases by a factor of ∼10, reaching the era of their formation at and beyond. These findings can be interpreted as evidence for an early epoch of star z ∼ 2 formation in the most massive galaxies and for ongoing star formation activity in lower mass galaxies.

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The FORS Deep Field: Field selection, photometric observations and photometric catalog

Cited by 82 publications

References 34 publications

Disk galaxy scaling relations at intermediate redshifts

Disk galaxy scaling relations at intermediate redshifts

Cluster galaxies in XMMU J2235-2557: galaxy population properties in most massive environments atz ~ 1.4

Specific Star Formation Rates to Redshift 5 from the FORS Deep Field and the GOODS-S Field

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