The Survey for Ionization in Neutral Gas Galaxies. II. The Star Formation Rate Density of the Local Universe

Hanish, D. J.; Meurer, G. R.; Ferguson, Henry C.; Zwaan, M. A.; Heckman, Timothy M.; Staveley‐Smith, L.; Bland-Hawthorn, Joss; Kilborn, V. A.; Koribalski, B. S.; Putman, Mary E.; Ryan-Weber, E. V.; Oey, M. S.; Kennicutt, Robert C.; Knezek, Patricia; Meyer, M.; Smith, R. C.; Webster, R. L.; Dopita, Michael A.; Doyle, M. T.; Drinkwater, Michael J.; Freeman, K. C.; Werk, Jessica K.

doi:10.1086/504681

Cited by 70 publications

(86 citation statements)

References 59 publications

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“…Similar values were calculated at z ∼ 0 from the SDSS (Brinchmann et al 2004;Nakamura et al 2004) and SINGG (Hanish et al 2006) projects, and from local volume studies (James et al 2008;Karachentsev & Kaisin 2010). Several authors extended local studies to redshifts z < 0.3 using optical spectroscopy (Tresse & Maddox 1998;Sullivan et al 2000).…”

Section: Introductionsupporting

confidence: 67%

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: Introductionsupporting

confidence: 67%

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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“…At z 0-6, we show the cosmic SFRD measurements compiled by Hopkins & Beacom (2006). The compilation of Hopkins & Beacom (2006) covers most of SFRD measurements made, to date, in various wavelength including Hα (Glazebrook et al 1999;Tresse et al 2002;Hanish et al 2006), mid-infrared (Flores et al 1999;Pérez-González et al 2005), submm (Barger et al 2000;Hughes et al 1998), radio (Condon et al 2002;Serjeant et al 2002), and X-ray (Georgakakis et al 2003). It also includes results of Giavalisco et al (2004b), Bunker et al (2004), andOuchi et al (2004) for z > 4 SFRDs estimated from UV luminosities.…”

Section: Cosmic Star Formation Historymentioning

confidence: 99%

LARGE AREA SURVEY FOR z = 7 GALAXIES IN SDF AND GOODS-N: IMPLICATIONS FOR GALAXY FORMATION AND COSMIC REIONIZATION*

Ouchi

Mobasher

Shimasaku

et al. 2009

ApJ

311

388

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We present results of our large area survey for z -band dropout galaxies at z = 7 in a 1568 arcmin 2 sky area covering the SDF and GOODS-N fields. Combining our ultra-deep Subaru/Suprime-Cam z -and y-band (λ eff = 1 μm) images with legacy data of Subaru and Hubble Space Telescope, we have identified 22 bright z-dropout galaxies down to y = 26, one of which has a spectroscopic redshift of z = 6.96 determined from Lyα emission. The z = 7 luminosity function yields the best-fit Schechter parameters of φ * = 0.69 +2.62 −0.55 × 10 −3 Mpc −3 , M * UV = −20.10 ± 0.76 mag, and α = −1.72 ± 0.65, and indicates a decrease from z = 6 at a > 95% confidence level. This decrease is beyond the cosmic variance in our two fields, which is estimated to be a factor of 2. We have found that the cosmic star formation rate density drops from the peak at z = 2-3 to z = 7 roughly by a factor of ∼10 but not larger than ∼100. A comparison with the reionization models suggests either that the universe could not be totally ionized by only galaxies at z = 7, or more likely that properties of galaxies at z = 7 are different from those at low redshifts having, e.g., a larger escape fraction ( 0.2), a lower metallicity, and/or a flatter initial mass function. Our SDF z-dropout galaxies appear to form 60 Mpc long filamentary structures, and the z = 6.96 galaxy with Lyα emission is located at the center of an overdense region consisting of four UV bright dropout candidates, which might suggest an existence of a well-developed ionized bubble at z = 7.

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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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The Survey for Ionization in Neutral Gas Galaxies. II. The Star Formation Rate Density of the Local Universe

Cited by 70 publications

References 59 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

LARGE AREA SURVEY FOR z = 7 GALAXIES IN SDF AND GOODS-N: IMPLICATIONS FOR GALAXY FORMATION AND COSMIC REIONIZATION*

How do galaxies acquire their mass?

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