The FORS Deep Field spectroscopic survey

Noll, Stefan; Mehlert, D.; Appenzeller, I.; Bender, Ralf; Böhm, A.; Gabasch, A.; Heidt, J.; Hopp, U.; Jäger, Klaus; Seitz, S.; Stahl, O.; Tapken, C.; Ziegler, B.

doi:10.1051/0004-6361:20034434

Cited by 66 publications

(152 citation statements)

References 68 publications

Supporting

Mentioning

138

Contrasting

Order By: Relevance

“…NP05). At least for the red galaxies in our sample, this interpretation is supported by the corresponding presence of UV nebular emission lines of lower strength (see Heckman et al 1998;Noll et al 2004) in the spectra of the same γ 34 < −2 galaxies.…”

Section: Narrow Spectroscopic Featuressupporting

confidence: 64%

“…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).…”

Section: The Fdf K20 and Gdds Samplesmentioning

confidence: 99%

See 1 more Smart Citation

GMASS ultradeep spectroscopy of galaxies at z ~ 2

Noll

Pierini

Cimatti

et al. 2009

A&A

Self Cite

109

166

View full text Add to dashboard Cite

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.

show abstract

Section: Narrow Spectroscopic Featuressupporting

confidence: 64%

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

Self Cite

109

166

View full text Add to dashboard Cite

show abstract

“…The UV spectral slope β can be used to derive the dust attenuation for local starburst galaxies (e.g., Calzetti et al 1994;Leitherer et al 1999) and has been adopted as a dust indicator for high redshifts galaxies (e.g., Noll et al 2004;Hathi et al 2008b;Finkelstein et al 2012;Bouwens et al 2014). The main reason is that the intrinsic UV slope depends weakly on metallicity and stellar populations for star-forming galaxies (e.g., Heckman et al 1998;Leitherer et al 1999).…”

Section: Resultsmentioning

confidence: 99%

The VIMOS Ultra Deep Survey: Lyαemission and stellar populations of star-forming galaxies at 2 < z < 2.5

Fèvre

Ilbert

Cassata

et al. 2016

A&A

View full text Add to dashboard Cite

The aim of this paper is to investigate spectral and photometric properties of 854 faint (i AB < ∼ 25 mag) star-forming galaxies (SFGs) at 2 < z < 2.5 using the VIMOS Ultra-Deep Survey (VUDS) spectroscopic data and deep multi-wavelength photometric data in three extensively studied extragalactic fields (ECDFS, VVDS, COSMOS). These SFGs were targeted for spectroscopy as a result of their photometric redshifts. The VUDS spectra are used to measure the UV spectral slopes (β) as well as Lyα equivalent widths (EW). On average, the spectroscopically measured β (-1.36 ± 0.02), is comparable to the photometrically measured β (-1.32 ± 0.02), and has smaller measurement uncertainties. The positive correlation of β with the spectral energy distribution (SED)-based measurement of dust extinction E s (B − V) emphasizes the importance of β as an alternative dust indicator at high redshifts. To make a proper comparison, we divide these SFGs into three subgroups based on their rest-frame Lyα EW: SFGs with no Lyα emission (SFG N ; EW ≤ 0 Å), SFGs with Lyα emission (SFG L ; EW > 0 Å), and Lyα emitters (LAEs; EW ≥ 20 Å). The fraction of LAEs at these redshifts is ∼10%, which is consistent with previous observations. We compared best-fit SED-estimated stellar parameters of the SFG N , SFG L and LAE samples. For the luminosities probed here (∼L * ), we find that galaxies with and without Lyα in emission have small but significant differences in their SED-based properties. We find that LAEs have less dust, and lower star-formation rates (SFR) compared to non-LAEs. We also find that LAEs are less massive compared to non-LAEs, though the difference is smaller and less significant compared to the SFR and E s (B − V). When we divide the LAEs according to their Spitzer/IRAC 3.6 μm fluxes, we find that the fraction of IRAC-detected (m 3.6 < ∼ 25 mag) LAEs is much higher than the fraction of IRAC-detected narrow band (NB)-selected LAEs at z 2-3. This could imply that UV-selected LAEs host a more evolved stellar population, which represents a later stage of galaxy evolution, compared to NB-selected LAEs.

show abstract

“…1 http://www.astro.caltech.edu/twiki_phat/bin/view/ Main/WebHome TEsting Program (STEP; Heymans et al 2006;Massey et al 2007) and led to important improvements in the methodology of measuring galaxy shapes for weak gravitational lensing applications. Similar but much more limited blind tests of photoz's have been performed by Hogg et al (1998) on spectroscopic data from the Keck telescope on the Hubble Deep Field (HDF), by Hildebrandt et al (2008) on spectroscopic data from the VIMOS VLT Deep Survey (VVDS; Le Fèvre et al 2004) and the FORS Deep Field (FDF; Noll et al 2004), and by Abdalla et al (2008b) on the sample of Luminous Red Galaxies from the SDSS-DR6.…”

Section: Introductionmentioning

confidence: 93%

PHAT: PHoto-zAccuracy Testing

Hildebrandt

Arnouts

Capak

et al. 2010

A&A

243

305

View full text Add to dashboard Cite

Context. Photometric redshifts (photo-z's) have become an essential tool in extragalactic astronomy. Many current and upcoming observing programmes require great accuracy of photo-z's to reach their scientific goals. Aims. Here we introduce PHAT, the PHoto-z Accuracy Testing programme, an international initiative to test and compare different methods of photo-z estimation. Methods. Two different test environments are set up, one (PHAT0) based on simulations to test the basic functionality of the different photo-z codes, and another one (PHAT1) based on data from the GOODS survey including 18-band photometry and ∼2000 spectroscopic redshifts.Results. The accuracy of the different methods is expressed and ranked by the global photo-z bias, scatter, and outlier rates. While most methods agree very well on PHAT0 there are differences in the handling of the Lyman-α forest for higher redshifts. Furthermore, different methods produce photo-z scatters that can differ by up to a factor of two even in this idealised case. A larger spread in accuracy is found for PHAT1. Few methods benefit from the addition of mid-IR photometry. The accuracy of the other methods is unaffected or suffers when IRAC data are included. Remaining biases and systematic effects can be explained by shortcomings in the different template sets (especially in the mid-IR) and the use of priors on the one hand and an insufficient training set on the other hand. Some strategies to overcome these problems are identified by comparing the methods in detail. Scatters of 4-8% in Δz/(1 + z) were obtained, consistent with other studies. However, somewhat larger outlier rates (>7.5% with Δz/(1 + z) > 0.15; >4.5% after cleaning) are found for all codes that can only partly be explained by AGN or issues in the photometry or the spec-z catalogue. Some outliers were probably missed in comparisons of photo-z's to other, less complete spectroscopic surveys in the past. There is a general trend that empirical codes produce smaller biases than template-based codes. Conclusions. The systematic, quantitative comparison of different photo-z codes presented here is a snapshot of the current state-ofthe-art of photo-z estimation and sets a standard for the assessment of photo-z accuracy in the future. The rather large outlier rates reported here for PHAT1 on real data should be investigated further since they are most probably also present (and possibly hidden) in many other studies. The test data sets are publicly available and can be used to compare new, upcoming methods to established ones and help in guiding future photo-z method development.

show abstract

The FORS Deep Field spectroscopic survey

Cited by 66 publications

References 68 publications

GMASS ultradeep spectroscopy of galaxies at z ~ 2

GMASS ultradeep spectroscopy of galaxies at z ~ 2

The VIMOS Ultra Deep Survey: Lyαemission and stellar populations of star-forming galaxies at 2 < z < 2.5

PHAT: PHoto-zAccuracy Testing

Contact Info

Product

Resources

About