The H<b>α</b>luminosity function and star formation rate up to<b>z ∼ 1</b>

Tresse, L.; Maddox, S.; Fèvre, O. Le; Cuby, Jean-Gabriel

doi:10.1046/j.1365-8711.2002.05919.x

Cited by 110 publications

(201 citation statements)

References 44 publications

(107 reference statements)

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“…4. The uncertainties in the structural parameters were taken from van der Wel et al (2012). There is a clear contrast between the galaxies CANDELS 15784, 16155, and 19256, which have Sérsic indexes of n ∼ 2-3, and the rest, which have n < 1.5.…”

Section: Morphologiesmentioning

confidence: 99%

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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: Morphologiesmentioning

confidence: 99%

“…In the mentioned redshift gap 0.5 < z < 0.8 in Hα-based studies, we only find a few objects in the lower limits of the NIR spectroscopic surveys indicated above. These limits are z > 0.5 (Tresse et al 2002), z > 0.77 (Doherty et al 2006), and z > 0.79 (Glazebrook et al 1999). No narrow-band surveys cover this gap.…”

Section: Introductionmentioning

confidence: 97%

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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“…Since our model does not (Thompson et al 2006). The red squares are Hα, Hβ and OII data (Hanish et al 2006;Pérez-González et al 2003;Tresse et al 2002;Hopkins et al 2000;Moorwood et al 2000;Sullivan et al 2000;Glazebrook et al 1999;Yan et al 1999;Tresse & Maddox 1998;Gallego et al 1995;Pettini et al 1998;Teplitz et al 2003;Gallego et al 2002;Hogg et al 1998;Hammer et al 1997). The orange squares are 1.4 GHz data (Mauch & Sadler 2007;Condon et al 2002;Sadler et al 2002;Serjeant et al 2002;Machalski & Godlowski 2000;Haarsma et al 2000;Condon 1989).…”

Section: Best-fit Model and Effects Of Physical Processesmentioning

confidence: 99%

How do galaxies acquire their mass?

Cattaneo

Mamon

Warnick

et al. 2011

A&A

122

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We study the growth of galaxy masses, via gas accretion and galaxy mergers. We introduce a toy model that describes (in a single equation) how much baryonic mass is accreted and retained into galaxies as a function of halo mass and redshift. In our model, the evolution of the baryons differs from that of the dark matter because 1) gravitational shock heating and AGN jets suppress gas accretion mainly above a critical halo mass of M shock ∼ 10 12 M ; 2) the intergalactic medium after reionisation is too hot for accretion onto haloes with circular velocities v circ < ∼ 40 km s −1 ; 3) stellar feedback drives gas out of haloes, mainly those with v circ < ∼ 120 km s −1 . We run our model on the merger trees of the haloes and sub-haloes of a high-resolution dark matter cosmological simulation. The galaxy mass is taken as the maximum between the mass given by the toy model and the sum of the masses of its progenitors (reduced by tidal stripping). Designed to reproduce the present-day stellar mass function of galaxies, our model matches fairly well the evolution of the cosmic stellar density. It leads to the same z = 0 relation between central galaxy stellar and halo mass as the one found by abundance matching and also as that previously measured at high mass on SDSS centrals. Our model also predicts a bimodal distribution (centrals and satellites) of stellar masses for given halo mass, in very good agreement with SDSS observations. The relative importance of mergers depends strongly on stellar mass (more than on halo mass). Massive galaxies with m stars > m crit ∼ Ω b /Ω m M shock ∼ 10 11 M acquire most of their final mass through mergers (mostly major and gas-poor), as expected from our model's shutdown of gas accretion at high halo masses. However, although our mass resolution should see the effects of mergers down to m stars 10 10.6 h −1 M , we find that mergers are rare for m stars 10 11 h −1 M . This is a consequence of the curvature of the stellar vs. halo mass relation set by the physical processes of our toy model and found with abundance matching. So gas accretion must be the dominant growth mechanism for intermediate and low mass galaxies, including dwarf ellipticals in clusters. The contribution of galaxy mergers terminating in haloes with mass M halo < M shock (thus presumably gas-rich) to the mass buildup of galaxies is small at all masses, but accounts for the bulk of the growth of ellipticals of intermediate mass (∼10 10.5 h −1 M ), which we predict must be the typical mass of ULIRGs.

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“…To estimate the number of Hα emitters present in our WIRCam image, we use the Hα luminosity function of Tresse et al (2002) without reddening correction. To our detection limit, and assuming that the NB flux is dominated by the Hα line flux, we estimate that we have ∼300 Hα emitters in the redshift interval [0.607-0.623].…”

Section: Low Redshift Emittersmentioning

confidence: 99%

Limits on the luminosity function of Lyαemitters atz= 7.7

Hibon

Cuby

Willis

et al. 2010

A&A

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101

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Aims. The Lyα luminosity function (LF) of high-redshift Lyα emitters (LAEs) is one of the few observables of the re-ionization epoch accessible with 8-10 m class telescopes. The evolution of the LAE LF with redshift is dependent upon the physical evolution of LAEs and the ionisation state of the Universe towards the end of the Dark Ages. Methods. We performed a narrow-band imaging program at 1.06 μm using CFHT/WIRCam. The observations target Lyα emitters at redshift z ∼ 7.7 in the CFHT-LS D1 field. From these observations we derived a photometric sample of 7 LAE candidates at z ∼ 7.7. Results. We derive luminosity functions for the full sample of seven objects and for subsamples of four objects. Assuming the brightest objects in our sample are real, we find that the resulting luminosity function is not consistent with previous work at lower redshifts. More definitive conclusions will require spectroscopic confirmation.

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The Hαluminosity function and star formation rate up toz ∼ 1

Cited by 110 publications

References 44 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

How do galaxies acquire their mass?

Limits on the luminosity function of Lyαemitters atz= 7.7

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