Star forming rates between <i>z</i> = 0.25 and <i>z</i> = 1.2 from the 
CADIS emission line survey

Hippelein, H.; Maier, C.; Meisenheimer, K.; Wolf, Christian; Fried, J. W.; Kuhlmann, B. von; Kümmel, M.; Phleps, S.; Röser, H.-J.

doi:10.1051/0004-6361:20021898

Cited by 97 publications

(141 citation statements)

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“…Gunawardhana et al (2013Gunawardhana et al ( , 2015 have recently combined SDSS data with deeper optical spectroscopy from the GAMA survey to z < 0.35. Analogously, other authors obtained SFRDs with a narrow-band technique at z ∼ 0.24 (Pascual et al 2001;Fujita et al 2003;Hippelein et al 2003;Pascual 2005;Westra & Jones 2008;Shioya et al 2008;Morioka et al 2008;Westra et al 2010) and z ∼ 0.4 (Glazebrook et al 2004;Pascual 2005). Other surveys collected large samples of objects with this technique within redshift slices up to z < 0.4 (Ly et al 2007;Dale et al 2010).…”

Section: Introductionmentioning

confidence: 85%

Properties of galaxies at the faint end of the Hαluminosity function atz~ 0.62

Gómez-Guijarro

Gallego

Villar

et al. 2016

A&A

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Context. Studies measuring the star formation rate density, luminosity function, and properties of star-forming galaxies are numerous. However, it exists a gap at 0.5 < z < 0.8 in Hα-based studies. Aims. Our main goal is to study the properties of a sample of faint Hα emitters at z ∼ 0.62. We focus on their contribution to the faint end of the luminosity function and derived star formation rate density, characterising their morphologies and basic photometric and spectroscopic properties. Methods. We use a narrow-band technique in the near-infrared, with a filter centred at 1.06 µm. The data come from ultra-deep VLT/HAWK-I observations in the GOODS-S field with a total of 31.9 h in the narrow-band filter. In addition to our survey, we mainly make use of ancillary data coming from the CANDELS and Rainbow Cosmological Surveys Database, from the 3D-HST for comparison, and also spectra from the literature. We perform a visual classification of the sample and study their morphologies from structural parameters available in CANDELS. In order to obtain the luminosity function, we apply a traditional V/V max method and perform individual extinction corrections for each object to accurately trace the shape of the function. Results. Our 28 Hα-selected sample of faint star-forming galaxies reveals a robust faint-end slope of the luminosity function α = −1.46 +0.16 −0.08 . The derived star formation rate density at z ∼ 0.62 is ρ SFR = 0.036 +0.012 −0.008 M yr −1 Mpc −3 . The sample is mainly composed of disks, but an important contribution of compact galaxies with Sérsic indexes n ∼ 2 display the highest specific star formation rates. Conclusions. The luminosity function at z ∼ 0.62 from our ultra-deep data points towards a steeper α when an individual extinction correction for each object is applied. Compact galaxies are low-mass, low-luminosity, and starburst-dominated objects with a light profile in an intermediate stage from early to late types.

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Section: Introductionmentioning

confidence: 85%

Properties of galaxies at the faint end of the Hαluminosity function atz~ 0.62

Gómez-Guijarro

Gallego

Villar

et al. 2016

A&A

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“…The tuneable filter technique has not been much employed previously in this field. A heroic attempt, includes the CADIS survey of emission line galaxies measuring SFRs between z = 0.25 and z = 1.2 (Hippelein et al 2003).…”

Section: Description Of the Programme And Design Of The Observationsmentioning

confidence: 99%

OMEGA – OSIRIS Mapping of Emission-line Galaxies in A901/2 – I. Survey description, data analysis, and star formation and AGN activity in the highest density regions

Chies-Santos

Pino

Aragón-Salamanca

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We present an overview of and first results from the OMEGA survey: the OSIRIS Mapping of Emission-line Galaxies in the multi-cluster system A901/2. The ultimate goal of this project is to study star formation and AGN activity across a broad range of environments at a single redshift. Using the tuneable-filter mode of the OSIRIS instrument on GTC, we target Hα and [Nii] emission lines over a ∼ 0.5 × 0.5 deg 2 region containing the z ∼ 0.167 multi-cluster system A901/2. In this paper we describe the design of the survey, the observations and the data analysis techniques developed. We then present early results from two OSIRIS pointings centred on the cores of the A901a and A902 clusters. AGN and star-forming (SF) objects are identified using the [Nii] / Hα vs. W Hα (WHAN) diagnostic diagram. The AGN hosts are brighter, more massive, and possess earlier-type morphologies than SF galaxies. Both populations tend to be located towards the outskirts of the high density regions we study. The typical Hα luminosity of these sources is significantly lower than that of field galaxies at similar redshifts, but greater than that found for A1689, a rich cluster at z ∼ 0.2. The Hα luminosities of our objects translate into star-formation rates (SFRs) between ∼ 0.02 and 6 M yr −1 . Comparing the relationship between stellar mass and Hα-derived SFR with that found in the field indicates a suppression of star formation in the cores of the clusters. These findings agree with previous investigations of this multi-cluster structure, based on other star formation indicators, and demonstrate the power of tuneable filters for this kind of study.

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“…Unfortunately, at distances greater than z ∼ 0.4, this line redshifts out of the optical and into the near-IR portion of the spectrum, where it is much more difficult to observe (e.g., Glazebrook et al 2004). Consequently, by z ∼ 1, the [O ii] λ3727 emission line, which is produced by collisional excitation, has taken the place of Hα (e.g., Hippelein et al 2003;Ly et al 2007), and by z 2, the preferred indicator of star formation is the rest-frame ultraviolet continuum (e.g., Pettini et al 2001;Hopkins 2004). Like the emission-line indicators, the rest-frame UV directly traces the flux of young, massive stars, but in this case, the timescale over which the star formation is measured is ∼100 Myr, and the result is much more sensitive to internal extinction.…”

Section: Introductionmentioning

confidence: 99%

“…Others are based on narrow-band surveys of selected high redshift (z > 0.8) epochs, and are thus only sensitive to high equivalent width objects (e.g., Ly et al 2007;Takahashi et al 2007). Still others employ near-IR Fabry-Perot observations and are restricted to the very brightest (∼1 dex) [O ii] emitters at z ∼ 1 (Hippelein et al 2003). Consequently, while the local (z < 0.2) [O ii] luminosity function is reasonably well defined (Gallego et al 1996;Gilbank et al 2010), measurements of the evolution of [O ii] λ3727 emission over the last ∼5 Gyr of cosmic time are rather limited.…”

Section: Introductionmentioning

confidence: 99%

THE HETDEX PILOT SURVEY. IV. THE EVOLUTION OF [O II] EMITTING GALAXIES FROMz∼ 0.5 TOz∼ 0

Ciardullo

Grönwall

Adams

et al. 2013

ApJ

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We present an analysis of the luminosities and equivalent widths of the 284 z < 0.56 [O ii]-emitting galaxies found in the 169 arcmin 2 pilot survey for the Hobby-Eberly Telescope Dark Energy Experiment (HETDEX). By combining emission-line fluxes obtained from the Mitchell spectrograph on the McDonald 2.7 m telescope with deep broadband photometry from archival data, we derive each galaxy's dereddened [O ii] λ3727 luminosity and calculate its total star formation rate. We show that over the last ∼5 Gyr of cosmic time, there has been substantial evolution in the [O ii] emission-line luminosity function, with L * decreasing by ∼0.6 ± 0.2 dex in the observed function, and by ∼0.9 ± 0.2 dex in the dereddened relation. Accompanying this decline is a significant shift in the distribution of [O ii] equivalent widths, with the fraction of high equivalent-width emitters declining dramatically with time. Overall, the data imply that the relative intensity of star formation within galaxies has decreased over the past ∼5 Gyr, and that the star formation rate density of the universe has declined by a factor of ∼2.5 between z ∼ 0.5 and z ∼ 0. These observations represent the first [O ii]-based star formation rate density measurements in this redshift range, and foreshadow the advancements which will be generated by the main HETDEX survey.

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Star forming rates between z = 0.25 and z = 1.2 from the CADIS emission line survey

Cited by 97 publications

References 47 publications

Properties of galaxies at the faint end of the Hαluminosity function atz~ 0.62

Properties of galaxies at the faint end of the Hαluminosity function atz~ 0.62

OMEGA – OSIRIS Mapping of Emission-line Galaxies in A901/2 – I. Survey description, data analysis, and star formation and AGN activity in the highest density regions

THE HETDEX PILOT SURVEY. IV. THE EVOLUTION OF [O II] EMITTING GALAXIES FROMz∼ 0.5 TOz∼ 0

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